Open Access

Ionospheric current contribution to the main impulse of a negative sudden impulse

  • Geeta Vichare1Email author,
  • Rahul Rawat1,
  • Ankush Bhaskar1 and
  • Bashir M Pathan1
Earth, Planets and Space201466:92

https://doi.org/10.1186/1880-5981-66-92

Received: 6 December 2013

Accepted: 29 July 2014

Published: 18 August 2014

Abstract

The geomagnetic field response to a moderate-amplitude negative sudden impulse (SI) that occurred on 14 May 2009 at 10:30 UT was examined at 97 geomagnetic observatories situated all over the globe. The response signature contains a contribution from magnetospheric as well as ionospheric currents. The main impulse (MI) is defined as the maximum depression in the observed geomagnetic field. It is observed that for low-to-high latitudes, the amplitude of the MI is larger in the afternoon to post-dusk sector than in the dawn-noon sector, indicating asymmetry in the MI amplitude. We estimated the contribution at various observatories due to the Chapman-Ferraro magnetopause currents using the Tsyganenko model (T01) and subtracted this from the observed MI amplitude to obtain the contribution due to ionospheric currents. It is found that the ionospheric currents contribute significantly to the MI amplitude of moderate SI even at low-to-mid latitudes and that the contribution is in the same direction as that from the magnetopause currents near dusk and in the opposite direction near dawn. The equivalent current vectors reveal a clockwise (anticlockwise) ionospheric current loop in the afternoon (morning) sector during the MI of the negative pressure impulse. This evidences an ionospheric twin-cell-vortex current system (DP2) due to field-aligned currents (FACs) associated with the dusk-to-dawn convection electric field during the MI of an SI. We also estimated the magnetic field variation due to prompt penetration electric fields, which is found to be very small at low latitudes in the present case. The studied SI is not associated with shock, and hence no preliminary reverse impulse was evident. In addition, the summer hemisphere reveals larger MI amplitudes than the winter hemisphere, indicating once again the role of ionospheric currents.

Background

A sudden enhancement/drop in solar wind dynamic pressure causes the sudden compression/expansion of the magnetosphere, forming a positive/negative sudden impulse (SI) in the geomagnetic field (Nishida and Jacobs 1962). The signatures of these impulses in the ground magnetic field are quite complex due to the contributions from several current systems flowing in the magnetosphere and ionosphere. Using rapid-run magnetograms, it has been observed that the geomagnetic response signature of an SI is preceded by an initial rapid variation. The broad features of the geomagnetic signature include a first rapid response, also known as a preliminary impulse (PI) with a time scale of a few seconds to a few minutes, followed by a main impulse (MI). Araki (1977) described the geomagnetic signature of SIs in terms of a preliminary impulse of polar origin (DPpi), a main impulse dominating at low latitude (DLmi), and a main impulse of polar origin (DPmi). The PI is further categorized into positive and negative PIs. If the PI is negative (positive) during enhanced (reduced) solar dynamic pressure, then it is known as a preliminary reversed impulse (PRI). The DL field is a stepwise change in the geomagnetic field, and the DP field is a bipolar type. In this paper, we define the MI of a negative SI as the maximum reduction in the total field containing DPpi, DLmi, and DPmi parts.

Over the past six decades, several studies have been dedicated to understanding the characteristics of SIs (Sugiura 1953; Nagata and Abe 1955; Matsushita 1962; Sano 1962; Tamao 1964; Nishida et al. 1966; Rastogi and Sastri 1974; Araki et al. 1985, 2006; Araki and Nagano 1988; Araki 1994; Sastri et al. 1995; Yamada et al. 1997; Takeuchi et al. 2000, 2002a; Villante and Di Giuseppe 2004; Huang et al. 2008; Shinbori et al. 2009; Wang et al. 2009). Based on the magnetic field observations on ground, an equivalent ionospheric current system for the PI has been deduced (Araki et al. 1985; Araki 1994), which is similar to the DP2 current system (Nishida et al. 1966). This current system consists of twin-vortex type ionospheric currents generated by field-aligned currents (FACs) that give a bipolar signature on the ground (Araki 1994). The MI signature mainly comprises contribution due to currents flowing at the magnetopause and transient currents generated in the ionosphere and magnetosphere. Rastogi and Sastri (1974) found that the equatorial enhancement is larger for a PRI than for an MI, highlighting the stronger role of ionospheric conductivity in a PRI than that during an MI. Attempts have been made to study the local time (LT) variation of MI amplitude; for example, Shinbori et al. (2009) studied this variation statistically. However, not many studies have been carried out to investigate the LT variation for an individual SI. Gaining an understanding of this is important, as the results may differ for various SI events because the geomagnetic field response to SIs strongly depends on factors such as the orientation and magnitude of the interplanetary magnetic field (Wing and Sibeck 1997; Lee and Lyons 2004), orientation of shocks/discontinuities (Takeuchi et al. 2002b; Wang et al. 2006), the value of pressure before disturbance, and the change in pressure amplitude (Borodkova et al. 2006). Therefore, any statistical studies performed without consideration of these aspects may be unable to provide a true picture of the LT variation, which indicates the importance of case studies.

It has been estimated that the time required for a plasma front to sweep past the geomagnetic field is not more than 30 s, but the observed rise time of SIs is a few minutes. According to the model presented by Dessler et al. (1960), a negative correlation between SI amplitude and rise time can be expected because the larger the distance of the SI source from the observer, the longer the rise time and the smaller the amplitude due to attenuation. The time duration of SI depends on the following: the time taken by the shock front or discontinuity to sweep the geoeffective distance along the magnetosphere, the thickness of the shock front or the discontinuity in the solar wind, inertia of the magnetospheric plasma, and the broadening of the wave front during the passage through the magnetosphere (Nishida 1966). Wang et al. (2006) statistically investigated the effect of the interplanetary shock strength and orientation on SI rise time and found that oblique shocks result in a longer rise time of SIs.

Nishida and Jacobs (1962) noticed a similarity between positive and negative SIs and claimed that any theory of positive impulse (SI+) should be able to explain the phenomenon of negative impulse (SI) in an opposite sense. In support of this, several studies investigating geomagnetic field response to the negative solar dynamic pressure pulses reported that the response is opposite to that of the positive impulse (Rastogi and Sastri 1974; Araki and Nagano 1988; Sastri et al. 1995; Takeuchi et al. 2000), which indicated that negative SIs can be explained by the physical model used for positive impulses but with reversed current systems. The numerical simulation of a moderate amplitude SI using solar wind-magnetosphere-ionosphere MHD model by Fujita et al. (2004) showed that the SI is basically a mirror image of the SI+. However, Fujita et al. (2012) later revisited the simulations with larger amplitude SI and concluded that SIand SI+ are not in a mirror image relation. They listed a few differences between SI and SI+, such as the overshielding of the convection electric field occurring in the MI phase of a negative SI event and in the PI phase of SI+, but the duration of the shielding for SI+ being shorter than that for the SI. Using SuperDARN data, Hori et al. (2012) observed differences in the ionospheric flow during SI and SI+, and Takeuchi et al. (2000, 2002a) also reported that the polarization distribution of SI is not opposite to that of SI+. Thus, various studies carried out during the last decade have pointed out differences between positive and negatives SIs, and have demonstrated that an SI is not simply mirror image of an SI+.

Tamao (1964) proposed the mechanism of an equivalent current system for a PRI, based on the three-dimensional propagation of hydromagnetic waves in cold plasma, whereas Kikuchi and Araki (1979) proposed the Earth-ionosphere waveguide TM0 mode as a mechanism of propagation of polar electric fields to the equator and applied this to the PRI occurrence at the equator. Tamao (1964) model suggested that the direct source of the PRI is an ionospheric Hall-current system caused by the incidence of mixed transverse hydromagnetic waves (pure transverse plus converted transverse), and Chi et al. (2001) observed a very good agreement between the observed rise time of the PRI and the rise time calculated using Tamao’s (1964) model. However, according to Kikuchi and Araki (2002), Tamao’s (1964) model cannot be applied at low latitudes because the rotational electric fields of the converted transverse mode do not generate the Hall currents that close in the ionosphere. They also pointed out that the Hall currents accompany the Pedersen currents in a collision-dominated ionosphere, and therefore the energy dissipated by the Pedersen currents could not be supplied by the converted transverse mode. Therefore, although both models predict and explain a few features of an SI, it appears that a more detailed investigation is required to resolve the issues described above.

This paper presents a case study of a single SI event using all available ground-based geomagnetic observatories and geosynchronous satellite observations to enable an understanding of the characteristics of the geomagnetic field response to the negative solar wind pressure impulse. This paper is presented as follows: firstly in ‘Database’ section, we introduce the event of a negative solar wind pressure impulse along with other solar wind and interplanetary parameters. ‘Observation’ section presents the response to the SI at geosynchronous satellites and at various ground observatories, and ‘Results and discussion’ section describes the characteristics of the SI, such as the contribution due to sudden changes in IMF, local time variation of the MI amplitude and duration, equivalent ionospheric currents during the MI phase, latitudinal variation of MI amplitude, hemispheric asymmetry, and the geomagnetic response after attaining maximum depression. Finally, ‘Conclusions’ section discusses and summarizes the findings of the present investigation.

Methods

Database

This study utilized 1-min time resolution geomagnetic data downloaded from the INTERMAGNET website (http://www.intermagnet.org). Digital fluxgate data with a 1-min resolution from the World Data Center of Geomagnetism, Kyoto and from a chain of observatories in the Indian longitude zone were also used. Table 1 lists the observatories along with their geographic latitude and longitude and geomagnetic latitudes. In addition to ground magnetic observations, magnetic data from geosynchronous satellites GOES-10, GOES-11, and GOES-12 were utilized.
Table 1

List of geomagnetic observatories

Sr No

Station Code

Geographic Lat (°)

Geographic Long (°E)

Geomagnetic Lat (°)

Sr No

Station Code

Geographic Lat (°)

Geographic Long (°E)

Geomagnetic Lat (°)

1

EBR

40.8

0.5

43.1

50

MIZ

39.1

141.2

30.6

2

CLF

48.0

2.3

49.8

51

ESA

39.2

141.4

30.7

3

DOU

50.1

4.6

51.4

52

CBI

27.1

142.2

18.7

4

TAM

22.8

5.5

24.7

53

MMB

43.9

144.2

35.4

5

MAB

50.3

5.7

51.4

54

GUA

13.6

144.9

5.3

6

WNG

53.7

9.1

54.1

55

CTA

−20.1

146.3

−28.0

7

NGK

52.1

12.7

51.9

56

CNB

−35.3

149.4

−42.7

8

BDV

49.1

14.0

48.8

57

MCQ

−54.5

159.0

−60.1

9

UPS

59.9

17.4

58.5

58

EYR

−43.4

172.4

−47.1

10

THY

46.9

17.9

46.0

59

SHU

55.4

199.5

54.4

11

HRB

47.9

18.2

46.9

60

HON

21.3

202.0

21.6

12

LYC

64.6

18.7

62.7

61

BRW

71.3

203.4

69.8

13

HLP

54.6

18.8

53.2

62

PPT

−17.6

210.4

−15.1

14

ABK

68.4

18.8

66.1

63

CMO

64.9

212.1

65.4

15

HER

−34.4

19.2

−34.0

64

SIT

57.1

224.7

60.3

16

BEL

51.8

20.8

50.2

65

VIC

48.5

236.6

54.1

17

LVV

49.9

23.8

47.9

66

FRN

37.1

240.3

43.5

18

PAG

42.5

24.2

40.6

67

NEW

48.3

242.9

54.9

19

NUR

60.5

24.7

57.9

68

YKC

62.5

245.5

68.9

20

SOD

67.4

26.6

64.0

69

MEA

54.6

246.7

61.6

21

HBK

−25.9

27.7

−27.1

70

TUC

32.2

249.3

39.9

22

IZN

40.5

29.7

37.8

71

BOU

40.1

254.8

48.4

23

KIV

50.7

30.3

47.6

72

CBB

69.1

255.0

76.5

24

MOS

55.5

37.3

50.9

73

BLC

64.3

264.0

73.2

25

BOX

58.1

38.2

53.4

74

RES

74.7

265.1

82.8

26

AAE

9.0

38.8

5.4

75

FCC

58.8

265.9

67.9

27

TFS

42.1

44.7

36.8

76

BSL

30.4

270.4

40.1

28

MAW

−67.6

62.9

−73.2

77

FRD

38.2

282.6

48.4

29

ABG

18.6

72.9

10.4

78

OTT

45.4

284.4

55.6

30

GUL

34.1

74.4

25.6

79

HUA

−12.0

284.7

−2.1

31

JPR

26.9

75.8

18.4

80

THL

77.5

290.8

87.4

32

AAA

43.3

76.9

34.5

81

IQA

63.8

291.5

74.0

33

TIR

8.5

77.0

−0.1

82

SJG

18.1

293.9

28.3

34

NGP

21.2

79.1

12.3

83

TRW

−43.3

294.6

−33.3

35

PON

11.9

79.9

2.5

84

AIA

−65.2

295.7

−55.3

36

NVS

54.9

83.2

45.8

85

PST

−51.7

302.1

−41.7

37

LZH

36.1

103.8

26.1

86

GDH

69.3

306.5

78.6

38

IRT

52.2

104.5

41.9

87

KOU

5.2

307.3

14.9

39

PHU

21.0

106.0

10.8

88

LRV

64.2

338.3

69.2

40

GZH

23.0

112.5

12.9

89

MBO

14.4

343.0

20.1

41

LRM

−22.2

114.1

−32.4

90

GUI

28.3

343.6

33.8

42

GNA

−31.8

115.9

−41.9

91

ASC

−7.9

345.6

−2.4

43

BMT

49.7

116.2

30.1

92

VAL

51.9

349.8

55.8

44

TIK

71.6

129.0

65.3

93

SFS

36.7

354.1

39.9

45

KNY

31.4

130.9

22.2

94

HAD

51.0

355.5

53.9

46

KDU

−12.7

132.5

−22.0

95

SPT

39.5

355.7

42.8

47

ASP

−23.8

133.9

−32.9

96

ESK

55.3

356.8

57.8

48

KNZ

35.3

140.0

26.7

97

LER

60.1

358.8

62.0

49

KAK

36.2

140.2

27.4

     
The event analyzed in this study was associated with moderate solar wind density variations accompanied by sudden changes in the orientation of the interplanetary magnetic field (IMF). Figure 1 shows the solar wind (SW) and IMF parameters on 14 May 2009 between 10:00 and 17:00 UT. The IMF and solar wind data from the ACE satellite were downloaded from http://spidr.ngdc.noaa.gov and are displayed in the figure without correction for travel time delay. The solar wind number density dropped suddenly at 10:40 UT from 7/cc to 1/cc within 4 min, and the corresponding change in SW dynamic pressure was −1.41 nPa, a change of about 93%. It is important to note that before the drop, the SW density was not steady but was oscillating. The density drop took place in two steps: at the end of the sudden decrease, there was a small gap in the SW density data followed by a slight increase, and the density then remained almost constant until 15:15 UT when the sudden density enhancement took place. Thus, the present SI event was accompanied by an SI + event.
Figure 1

Solar wind and IMF parameters on 14 May 2009 between 10:00 and 17:00 UT. Bx, By, and Bz are interplanetary magnetic field components; PSWmag and PSWdyn are magnetic and dynamic pressures of the solar wind, respectively; VSW and NSW are the velocity and density of the solar wind recorded by ACE satellite (all parameters are displayed without correction for travel time delay). Bottom plot shows SYM-H index where the MI of the negative impulse is shown between two vertical lines.

A statistical study by Takeuchi et al. (2002a) reported that 50% of SI events occur in tandem with SI+ events. They found that interplanetary reversed shocks are not a primary cause of SI events. Instead, SI events are produced by rapid decreases in the solar wind dynamic pressure associated with a variety of interplanetary structures such as tangential discontinuities at high-low speed stream interfaces within co-rotating interaction regions (CIRs), the front boundaries of magnetic clouds, the rear boundaries of non-compressive density enhancements (NCDEs), the front boundary of a small-scale plasma hole, and earthward propagating shocks from the rear side of a solar flare (Takeuchi et al. 2002b; Rastogi et al. 2010). Takeuchi et al. (2002a) identified a pair of SI-SI+ associated with a small-scale plasma hole embedded in a CIR, close to a heliospheric current sheet (HCS) and parallel to the Parker spiral direction.

In the present case, the southward component of the interplanetary magnetic field (IMF Bz) suddenly turned northward during a negative impulse and then remained constant until a positive enhancement of the SW density took place, where IMF Bz rapidly turned southward. In addition, the negative and positive impulses were accompanied by sudden turnings of the X and Y components of the IMF. The magnetic pressure of SW remained high between SI and SI+, with discernible discontinuities at the edges. The interplanetary structure seems, therefore, to be bounded by tangential discontinuities. These characteristics of the IMF and the SW parameters may indicate that a cavity with a low-particle density was impinging on the Earth's magnetosphere. The scale length of the discontinuity appeared to be about 5.6 × 106 km. Using magnetic co-planarity, the orientation of the discontinuity (the angle between the discontinuity normal and the GSE X-axis) is estimated (Schwartz 1998) and was found to be parallel to the Parker spiral at 1 AU.

The bottom plot in Figure 1 depicts the SYM-H index that indicates a sudden drop at approximately 12:00 UT associated with a negative pressure pulse and an increase at 16:30 UT corresponding to a positive impulse. The MI signature during the SI is shown between the two vertical lines in the SYM-H plot. The amplitude of the negative impulse in the SYM-H is around −27 nT. The onset of the negative pulse starts at approximately 11:50 UT and attains a minimum after a time interval of approximately 11 min. Note that the fall time of 11 min on the ground is much longer than that seen by the ACE satellite (approximately three times as long). There is also a small increase seen in the SYM-H index immediately after the negative impulse. Note that a small increase appeared in the SW dynamic pressure just after the minima at 10:44 UT, but this increase appears to be very small compared to the corresponding increase seen in the SYM-H index. However, it should be noted that just after the decrease, the SW density data was not available for a few minutes, and hence it was not possible to obtain accurate information pertaining to the SW density variation during that time period. A positive impulse is seen in SYM-H at 16:30 UT with amplitude of around 10 nT and a rise time of approximately 10 min. It is also observed that 3-h kp values during the interval did not rise above the value of 3.

Observations

Magnetospheric response

Magnetic field variations in the geosynchronous orbit are plotted in Figure 2, where magnetic data with a 1-min resolution from three satellites (GOES-10, GOES-11, and GOES-12) was available during the event. At the time of the event, magnetic local times (MLT) were approximately 03:00, 07:00, and 08:00 at GOES-11, GOES-12, and GOES-10, respectively. Figure 2 shows all three components of the magnetic field (Hp, He, and Hn) and the magnitude of the total magnetic field vector (Ht). From Figure 2, it can be seen that the variation in the Hp component associated with the SI dominates over the other components during the daytime, while GOES-11 (located at 03:00 MLT) records comparable SI-related variations in all three components. The magnetic field variations due to the sudden solar wind pressure changes at the geosynchronous orbit are mainly of the compressional or rarefactional type and are represented by the Hp component (Wang et al. 2009). We therefore only discuss the Hp component of the magnetic field here. The response signature at a geosynchronous height is essentially a simple step-like decrease, and the amplitudes of the sudden negative impulse at 03:00, 07:00, and 08:00 MLT are −8, −19, and −25 nT, respectively. Thus, the magnitude increases during daytime, which is consistent with earlier observations at geosynchronous orbit (Kokubun 1983) and could be attributed to larger changes in the magnetopause currents at a sub-solar point (Villante and Piersanti 2011).
Figure 2

Geosynchronous magnetic field response to the negative SI. (a) GOES-11, (b) GOES-12, and (c) GOES-10 satellites. Hp, He, Hn, and Ht represent the components of the geomagnetic field parallel to the satellite's spin axis, earthward, normal to Hp & He, and total field, respectively.

Two features can be observed that occurred before the onset of the event at all three satellites: a gradual increase in the magnetic field and wavy structures. The fluctuating structures at GOES-12 and GOES-10 (both located in the nearby MLT zone in the morning hours) are similar, while those of GOES-11 (3:00 MLT) shows damped fluctuations, indicating daytime enhancement of the wavy structures. These observations can be attributed to the fluctuations riding on the steady increase of the solar wind dynamic pressure observed prior to the SI impulse (Figure 1).

As the ground magnetic observatory at Huancayo lies on the same meridian and equatorial plane as the GOES-12 satellite, we compare the magnetic field responses at these two locations. The amplitude of the MI at the HUA station is larger (approximately −50 nT) than at GOES-12 (approximately −19 nT), and the amplitude ratio of the satellite to the ground is 0.34, which is moderately smaller than that recorded by Kokubun (1983) (0:55 at 07:00 MLT). The fall time during a negative impulse at GOES-12 is approximately 6 min, which is longer than the SW density impulse duration (4 min) and shorter than that on the ground (approximately 11 min in SYM-H).

Ground-based observations

Figure 3a,b,c,d,e,f,g,h displays the horizontal field response to sudden magnetospheric rarefaction in various longitudinal sectors, for a period of 50 min from 11:40 to 12:30 UT on 14 May 2009, corresponding to local times ranging from 02:00 to 22:00. Each sub-figure shows a stacked plot of H-variations at different geomagnetic latitudes (displayed on the right side), and quiet time variations at each station are plotted in the background. Almost all the stations reveal a stepwise decrease in the horizontal component of the geomagnetic field (H). As SYM-H can be roughly considered representative of the average geomagnetic response, the onset time of the negative pressure impulse is determined from SYM-H index and is shown by vertical lines at 11:50 UT in Figure 3. Figure 3a displays four plots in the longitude belt between 210°E and 240°E that correspond to 02:10 to 04:10 MLT, and the geomagnetic latitudes of the stations in this longitude sector are 65°N, 60°N, 54°N, and 15°S. Note that in Figure 3a,b,c,f, the scales of the H amplitudes are different for high and mid-to-low latitudes. An examination of the response in various local times and latitudinal sectors shows a disparity in the response signature. Some of the plots show a small positive increase near the onset time (e.g., the polar stations in Figure 3b,c and at a few high-to-middle latitude stations in Figure 3d,e,f), which may indicate the occurrence of a PRI signature. While some plots show no initial increase (e.g., the plots in Figure 3a,g,h), some plots show a sudden drop with a very smooth decrease (Figure 3a,g,h), and in some plots this drop has a wavy structure. As stated in the ‘Background’ section, we refer to the sudden drop (or the duration from onset to maximum reduction) as the phase of the MI.It can be observed from Figure 1 that the decrease in the solar wind pressure took place in two steps. At certain locations, particularly where an initial positive variation (just after the onset) is observed, two clearly discernible steps are observed in the MI. It is possible that the initial positive type of variation prior to the second step separates the MI signature of the second negative impulse from that of the first impulse, resulting in two discrete MI signatures. Stations with no initial positive signature show a smooth decrease in the H component which could be due to MI signatures only associated with the two consecutive negative impulses. Therefore, in general, the wavy signatures seen at certain locations during the MI phase of a two-step negative impulse may suggest the existence of an initial positive signature.There is another aspect associated with the fluctuations observed before the onset and during the MI. Note that in Figure 3, some of the plots show oscillating structures before the onset time while other plots show no such fluctuations (e.g., plots in Figure 3g,h). As noted in Figure 1, the SW pressure was already oscillating before the sudden drop took place, and it is therefore possible that these oscillations are seen in the ground data. Interestingly, these oscillations are prominently observed during the daytime. In addition, when there is an absence of oscillations during an MI, there is also generally an absence of oscillations before the onset.
Figure 3

Transient variation of the H component in various local time sectors. (a-h) H field in various longitudinal sectors at different latitudes (indicated on the right), background curves shown by thin lines represent the average of three quiet days. The vertical line at 11:50 UT shows the onset time of the negative impulse (for details see text).

Also note that after the minimum, the geomagnetic field shows a positive variation in general and then tries to attain steady state. This variation after the maximum depression is also different at different locations and local time sectors.

Geomagnetic latitudinal belt between 40°N and 50°N

Figure 3 shows that the geomagnetic response to the SI varies with latitude and local time. In order to examine the LT variations of the response, we choose a narrow range of latitude between 40° and 50°, where a good number of stations were available. Figure 4 shows the stacked plots of D- (left-hand panel) and H- (right-hand panel) variations recorded at observatories essentially between the geomagnetic latitudes of 40°N and 50°N, although a couple of observatories that lie just outside this latitudinal range are also included. The MLTs at each station are displayed on the right side of the figure, and the plots are arranged with increasing MLT from bottom to top. As noticed in the previous sub-section, the geomagnetic field response to SI at certain locations has an initial positive variation, which may indicate the occurrence of PRI. However, the PRI has a very rapid and strong variation that only lasts a few seconds. It is possible that the 1-min time-averaged values used in the present analysis may not have been able to display larger variations of smaller time scales. Therefore, in this section, we depict 1-s values of the geomagnetic field at a few available stations, as highlighted by the blue color in the figure. We use five stations (FRD, CLF, TFS, NVS, and IRT) that are close to the dawn and dusk terminators, with 1-s resolution data. Stations from noon to dusk show an initial positive increase in the H component (right side panel) just after the onset, but the 1-s data do not evidence a clear intense enhancement in the amplitude of the positive increase. Therefore, it is not possible to confirm that the initial positive variation represents the PRI signature, and hence it is not possible to infer about the occurrence of the PRI.
Figure 4

Ground magnetic field variations between 40° and 50° geomagnetic latitude. D and H components at various MLTs (which are referred to on the right). The blue curves indicate variation with 1-s data resolution.

The D-variations (expressed in nanotesla) in the four lowest plots in the left-side panel with MLTs between 03:30 and 06:41 show an initial increase after the onset time, and thereafter a decrease. At 07:52 MLT, the southern hemispheric station PST shows a very small D-variation, and the stations beyond this MLT show a positive type of MI signature in the D component. Few stations show an initial very small decrease followed by an increase. The signature of the main impulse in the D component is observed to be negative after midnight to near dawn and positive from afternoon to post-dusk.Response waveforms in the H and D components show noticeable variations after the main impulse signature. The geomagnetic response signature in the H component shows a positive variation in general after achieving the minimum and then tries to attain a quasi-steady state. We call the first variation occurring immediately after the minimum the ‘after maximum deviation’ (AMD) variation. In actual fact, one more oscillation appears at a few stations after this variation, but it has a very weak amplitude. Similarly in the D component, a signature opposite to the main impulse is observed just after the maximum deviation. To define the various phases of the response waveform, we indicate points d1, d2, d3, h1, h2, and h3 in the topmost plots of Figure 4. The points indicated by a subscript 1 show the onset time, which is also indicated by a vertical dashed line, and is assumed to be same for all the plots. Points with subscripts 2 and 3 indicate the end of the MI and AMD, respectively.

The amplitude of the MI is defined as the maximum deviation of the magnetic field from its pre-SI value. Hence, the MI amplitude in the H component is the variation in the H component from the onset time to the time where H attains the minimum value (the H-variation roughly attains the minimum at approximately 11 to 13 min after the onset time). If the times at points h1, h2, and h3 are th1, th2, and th3, respectively, then the quantity defined by (H(th2) − H(th1)) represents the MI amplitudes in H. Similarly, if the times at points d1, d2, and d3 are td1, td2, and td3 respectively, then the quantities defined by (D(td2) − D(td1)) represent the MI amplitudes in the D component. The amplitude difference between points 2 and 3 gives the amplitude of the AMD, i.e., (H(th3) − H(th2)) and (D(td3) − D(td2)). The MI amplitude in the H-component is minimum (approximately −7 nT) near dawn and thereafter continues to increase throughout the afternoon sector, reaching a maximum (approximately −47 nT) near dusk (at 18:54 MLT).

Low-latitude region (between 10° and 40° geomagnetic latitude)

At low latitudes, the geomagnetic field response to the solar wind pressure change is often step-like due to the Chapman-Ferraro magnetopause currents and a propagating compressional wave front. Geomagnetic variations at low latitudes can be considered as remote to field-aligned, auroral ionospheric, and equatorial electrojet currents (Araki 1977, 1994). It has been found that a geomagnetic SI at low latitudes is proportional to the change of the square root of the solar wind pressure. Siscoe et al. (1968), Russell et al. (1994), and Takeuchi et al. (2002a) reported that the slope of the regression line is consistent during SI+ and SI events.

In this section, we investigate the geomagnetic response in the low-to-mid latitude region between 10° and 40° geomagnetic latitude by plotting the MLT variation of the MI amplitude in the H component (Figure 5). Note that in order to obtain sufficient MLT coverage, the low-latitude range is been widened up to 40°. As stated in the previous sub-section, the amplitude of the MI is defined as ΔH = H(th2) − H(th1), where th1 is the onset time of SI and th2 is the time when the amplitude of the SI attains its maximum negative value. Note that if more than one station is available at a given MLT, then the average of the amplitudes at those stations is used to represent the amplitude of the MI at that particular MLT. Figure 5 depicts the higher MI amplitude of the negative impulse in the afternoon to post-dusk sector (approximately −30 nT) and the minimum near dawn (approximately −10 nT), exhibiting a strong dawn-dusk asymmetry. According to the empirical formula derived by Russell et al. (1994), Δ H = k P sw 2 P sw 1 , the change in the H component during the presently studied negative impulse is around −16 nT during daytime (k = 18.4 nT/nPa1/2), and approximately −13.3 nT at nighttime (k = 14.9 nT/nPa1/2). Note that these estimates are simple approximate values used for the comparison, although the actual magnetic field variations at each location due to magnetopause currents are estimated in ‘MLT dependence of ionospheric current contribution in the MI amplitude’ section using an empirical model. The departure of the observed MI magnitude from these rough values can be due to the contribution of other current systems that develop in the magnetospheric and ionospheric domain during SIs. In general, the amplitude of the response in the pre-dawn sector is comparable to that due to changes in the solar wind pressure, and the variation is almost double due to a simple pressure impulse in the afternoon zone, suggesting an additional contribution from other transient currents present during the event. A statistical study of SIs by Shinbori et al. (2009) showed that at low-to-mid latitudes, the amplitude attains a minimum at around 08:00 MLT, then increases towards noon, peaks in the afternoon hours, and once again peaks at midnight. Unfortunately, data between 22:00 and 00.00 MLT was not available in this latitudinal range, and hence we are unable to examine the nighttime enhancement of the H amplitude as reported by Araki et al. (2006) and Shinbori et al. (2009). However, from Figure 5 it is possible to observe that the H amplitude attains a minimum near 07:30 MLT and is fairly high at around 19:00 MLT; thus, the overall local time variation depicted in Figure 5 matches very well with that reported by Shinbori et al. (2009).
Figure 5

MLT variation of MI amplitude during SI in low-to-mid latitude region (10° to 40° geomagnetic latitudes).

The differences in MI amplitude at dawn and dusk are quantified by defining the asymmetry index as
γ = MI dusk MI dawn MI dusk + MI dawn

where MIdawn (= −11 nT) and MIdusk (= −33 nT) are the minimum and maximum values of MI amplitudes at dawn and dusk respectively, which gives value of γ equal to 0.5 in the present case. The dawn-dusk asymmetry index computed by Shinbori et al. (2009) for low latitudes up to 27° is around 0.2 and suddenly increases to approximately 1.2 at 35° latitude (Figure four in Shinbori et al. (2009)), and the average over 10° to 40° latitude is around 0.6, which compares well with our case study.

Equatorial region

In this section, we present observations at equatorial stations from different MLT sectors. A list of five equatorial stations is displayed in Table 2 (geomagnetic latitude < ± 6°), together with geographic longitude and geomagnetic and dip latitudes. Figure 6a,b,c,d,e displays the geomagnetic field variations at HUA, ASC, AAE, TIR, and GUA, and the background variations shown by the thin lines represent the quiet time variation at a given station. The MLTs at HUA, ASC, AAE, TIR, and GUA were 07:00, 11:00, 14:40, 17:15, and 21:40, respectively. It can be seen that there is a small positive variation before the main negative impulse at HUA, while ASC, AAE, TIR, and GUA have a clear MI-type signature without an initial positive increase. We examined the 1-s resolution data from the HUA observatory and noticed no remarkable enhancement in the amplitude of the initial positive variation. It is therefore difficult to comment on whether the initial positive variation is related to PRI or it could be a part of the fluctuations seen in the SW density before the onset.
Table 2

Equatorial magnetic observatories

Station name

Station code

Geographic longitude

Geomagnetic latitude

Dip latitude

Addis Ababa

AAE

38.77°E

5.36°N

1.34°N

Tirunelveli

TIR

77.8°E

0.03°N

0.4°N

Guam

GUA

144.88°E

5.56°N

6.34°N

Huancayo

HUA

285°E

2.1°S

0.28°N

Ascension Island

ASC

345.62°E

2.57°S

24.65°S

Figure 6

Equatorial geomagnetic field response to the negative SI at different longitudes. Geomagnetic coordinates are mentioned at the top, and the background curves show the average quiet day pattern.

The amplitudes of MI at HUA, ASC, AAE, TIR, and GUA are 50, 23, 40, 23, and 23 nT, respectively. It is interesting to note that the amplitude of the MI at ASC, which is near magnetic noon (at 11:00 MLT), has an amplitude of much less than that at 07:00 MLT and at 14:40 MLT. However, this can be justified through the dip latitude of ASC, which is quite high (approximately 25° S), and hence it is located quite far from the dip equator and experiences very small ionospheric conductivity compared to the equatorial Cowling conductivity. While comparing the observations in a narrow belt of the equatorial zone, it is necessary to bear in mind that the Cowling conductivity gradients in the vicinity of the magnetic equator are very sharp, resulting in large amplitude differences within a few degrees of latitude. The geomagnetic latitude of HUA is 2.1°N, which is closer to the geomagnetic equator than AAE (5.36°N GMlat). Shinbori et al. (2009) found that the daytime enhancement of the normalized SI amplitude at 5° away from the magnetic equator (GAM) has a peak amplitude of less than half the value of that is found close to the magnetic equator (YAP). From their Figure one, at 07:00 MLT, YAP had a normalized amplitude of 1.5, which was comparable with that at near noon at GAM. It is therefore quite possible that the present observation of the larger MI amplitude at 07:00 MLT could be due to the fact that HUA is located closer to the geomagnetic equator than AAE. Thus, in view of the magnetic latitudes of the observatories, the differences in the MI amplitudes could be due to the sharp latitudinal gradients of Cowling conductivity in a narrow belt of the equatorial region. Further, the dip latitudes of HUA and TIR are almost same (both situated close to the dip equator) and are located near dawn and dusk respectively. A comparison of the MI amplitude at these two locations reveals larger MI amplitude at the near-dawn station, HUA, than that at the near-dusk station, TIR.

Results and discussion

Contribution due to sudden changes in the IMF

If the SIs are accompanied with sudden changes in the IMF, then it is possible that other factors such as magnetopause currents, FAC and ionospheric currents, effects associated with prompt penetration, and overshielding could also contribute to the geomagnetic response during the sudden SW pressure changes. Takeuchi et al. (2000) studied an SI, where ΔPsw = −6.44 nPa Δ P sw = 1.6 nPa resulted in an amplitude of −26 nT in the geomagnetic response on the ground. It should be remembered that for the present event, ΔPsw of −1.41 nPa Δ P sw = 0.9 nPa resulted in a variation of −27 nT in SYM-H. This indicates that there is an inconsistency in the amplitude of the geomagnetic response in the two cases, as a smaller amplitude response would be expected in our case due to a smaller change in the SW dynamic pressure. Also note that in both cases, there was a sudden northward turning of the IMF at the time of the sudden drop in the pressure. However, during the event studied by Takeuchi et al. (2000) on 13 May 1995, the IMF changed from a smaller value to a larger value of a northward IMF, while during the presently studied case on 14 May 2009, the sudden northward turning was from a southward direction to a northward IMF Bz. Recently, Bhaskar and Vichare (2013) have statistically shown that during a northward turning, in addition to the overshielding effects associated with R2 FACs, the reduction in the southward component contributes to the negative variation in the H component at equatorial stations during daytime. Therefore, it may be possible that for the presently studied case, there was a stronger negative contribution existing in the same direction as that due to the magnetopause currents during daytime and which may therefore have resulted in a larger decrease of the H component. In order to examine this possibility, we obtained the equatorial prompt penetration electric fields (PPE) from the ‘Real-time model of the Ionospheric Electric Fields’ (http://www.geomag.us/models/PPEFM/RealtimeEF.html). Figure 7 displays the PPE from the above-mentioned model at different LTs and clearly shows the presence of a westward electric field during daylight hours and an eastward electric field during the nighttime. Using ionospheric conductivity values from World Data Center (WDC), Kyoto, we estimated the magnetic field variations associated with PPE at low latitudes, which was found to be approximately −2 nT at 12:00 MLT. Thus, the magnetic field contribution due to PPE is very small for this event. In addition, we examined the ASYM-H index during the event and found this to be very high, which could be due to the presence of ionospheric currents (DP2) or the partial ring current associated with the FACs generated during the SI. Therefore, the difference in the geomagnetic field response between the present and earlier cases could be due to ionospheric currents associated with the FACs.
Figure 7

Modeled ionospheric prompt penetration electric field during MI of the SI at different LT sectors.

MLT dependence of ionospheric current contribution in the MI amplitude

The magnetic field response to sudden SW pressure changes comprises contributions from the Chapman-Ferraro magnetopause currents, ionospheric currents (such as the Pedersen currents and Hall currents), and field-aligned currents (FACs). Using the Tsyganenko empirical model, T01 (Tsyganenko 2002a,[b]), we compute the magnetic field produced by the Chapman-Ferraro currents at the location of each ground observatory. Figure 8a shows the MLT variation of the observed MI amplitude in the H component at the stations located between 60°S and 65°N geomagnetic latitudes, excluding the equatorial stations. Figure 8b shows the MLT variation of the contribution at corresponding stations due to the magnetopause currents using the T01 model for SW and IMF conditions identical to those occurred during the presently studied case, and Figure 8c shows the MLT profile of the residual field in the H component after subtracting the contribution from the magnetopause currents from the observed MI amplitude. The MLT variation of the model estimates of magnetopause current contribution is relatively weak, and hence the profile of the residual field is similar to that of the observed MI amplitude. It is believed that the residual fields essentially represent the contribution from the ionospheric currents and FACs. The model estimates of the contribution from the magnetopause currents attain a maximum near noon (Figure 8b), while the observed MI amplitude peaks near dusk (Figure 8a). Near dusk, the amplitude of the residual field is considerably larger than that due to Chapman-Ferraro current contribution and hence reveals the significance of the ionospheric currents and FACs. Note that near dawn, the observed MI amplitudes are slightly smaller than those due to the magnetopause currents, resulting in small positive values of the residual fields. The contribution due to the FACs is symmetrical at about noon and has the same direction as in the morning and in the afternoon sectors spanning from dawn to dusk (Araki et al. 2006) and, hence, will not introduce any asymmetry in the residual field between the two MLT sectors. Therefore, the ionospheric currents are the only candidates that could be responsible for the observed differences in the residual field in the morning and afternoon sectors. It can then be postulated that in the near-dawn sector, the magnetic field variations due to the ionospheric currents are in the opposite direction to those of the magnetopause currents, thus reducing the amplitude of the observed MI. Most of the MI amplitude near dawn is due to the magnetopause currents, and hence this delivers very small residual values, while the ionospheric current contribution is in the same direction as that of the magnetospheric currents near dusk, thereby enhancing the amplitude of the observed MI.
Figure 8

MLT variations. (a) MI amplitude, ΔH; (b) estimate of magnetic field variations due to magnetopause currents, ΔHMP; and (c) residual field, ΔH − ΔHMP. For stations with geomagnetic latitudes between 60°S and 65°N.

Equivalent current system during the MI

Figure 9 shows the equivalent current vectors during the MI of the negative impulse, which are derived from the residual magnetic field variations in the H and D components during the main impulse, at the magnetic observatories located between the north pole and 35°N geomagnetic latitude (concurrent circles are drawn at 15° spacing). The residual magnetic field is obtained by subtracting the magnetopause current contribution from the observed MI amplitude. Note that here we consider only those stations where there was a distinct MI signature in both H and D components. The current vectors indicate the presence of a counterclockwise vortex near dawn and a clockwise vortex in the afternoon sector, although the centers of both the loops are not apparent. Thus, Figure 9 clearly demonstrates a two-cell current system during the main impulse of the SI.
Figure 9

Equivalent current vectors (red arrows) during the main impulse of SI event on 14 May 2009.

Local time dependence of the time duration of the MI

The ‘time duration’ (or fall time) of the MI is the time interval between the onset time and the end of the MI (th2-th1). From Figure 4, it can be noted that the duration of the MI changes with the local time, and hence in this section, we plot the LT variation of the duration of the MI in the H component for all stations (Figure 10). We also estimate the MI duration using another method where instead of using the minimum in the H component, we take the intersection of the line fits before and after the minimum. Estimates from these two methods show a similar LT dependence. In general, the scatter plot and the 2-h average curve (solid line) show smaller values of the MI interval during the daytime compared to the nighttime. This is in accordance with the observations by Ondoh (1963) who showed that the time duration of both positive and negative SIs is shorter in the daytime than in the nighttime. In addition, it can be noted that the interval is smaller during the afternoon hours compared to during the morning time.
Figure 10

Local time variation of the MI time duration. Solid curve represents 2-h averaged values.

Latitudinal variation of MI amplitude

As noticed in the previous sections, the MI amplitude varies with local time. In order to study the latitudinal dependence, we separate the two LT zones (dawn to near noon and from dusk to pre-midnight). Figure 11 shows the variation of the MI amplitude in the H component in relation to the geomagnetic latitude in both these local time sectors. Here, we only depict variations in the northern hemisphere to avoid possible complications related to interhemispheric differences. Unfortunately, the LT zone from dusk to pre-midnight has a very limited latitudinal coverage, but the local time sector from dawn to near noon (up to 14:30 MLT) covers a wider latitudinal range, from low-to-near-polar latitudes. It can be noticed that in the mid latitude range, the amplitude in the dusk to pre-midnight sector is higher than in the dawn to noon sector, which supports the observations presented in the previous section. The latitudinal variation in the dawn to noon sector shows that the MI amplitude increases significantly after 50°N latitude (and it can be noted that one point near 73°N displays the maximum amplitude).
Figure 11

Latitudinal variation of MI amplitude in dawn to near noon and dusk to pre-midnight sectors.

Magnetic field variations after maximum deviation

As mentioned in ‘Ground-based observations’ section, most of the geomagnetic response profiles show variations after attaining a peak in the negative amplitude. We measure the amplitude of this variation wherever the variation is clearly detectable and refer to this as the 'after maximum deviation' (AMD). In ‘Conclusions’ section, we shall discuss the waveform of the total magnetic field obtained from the superimposed magnetopause and ionospheric currents, which clearly demonstrates the existence of an AMD, and hence it is part of the SI response. However, it can be noticed from Figure 1 that after the main decrease of SW pressure, there was a small enhancement in the ACE data. The SW pressure was 0.1 nPa at the end of the main decrease but then reached 0.22 nPa after a few minutes. The estimated magnetic field variation associated with this pressure change is approximately 2 to 3 nT on the ground, which is very small compared to the observed amplitudes of the AMD variations. It is also important to note that the AMD signature is associated with almost steady interplanetary conditions, with a steady northward IMF, and hence there is no contribution from overshielding or penetration electric fields. It can therefore be assumed that the AMD variations are not associated with the external driver.

Figure 12 shows the scatter plots between MI and AMD amplitudes (scatter plots for H and D components are shown in Figure 12a,b, respectively). Note that here we do not consider the stations where the AMD variation is not clear or where it is flat. These plots depict a very good anti-correlation between the MI and AMD amplitudes in both components (correlation = −0.97 and −0.88 for H and D, respectively), suggesting a relationship between these two quantities. The least square fits have slopes equal to −0.94 and −0.53 for the H and D components, respectively. The magnitudes of the slopes (<1) indicate damped amplitudes of AMDs, although they are proportional to the MI amplitude. Recently, a new feature of the ionospheric flow variations after the main impulse of SI was noticed in the SuperDARN observations (Hori et al. 2012) and also in simulations (Yu and Ridley 2011; Fujita et al. 2012). Hori et al. (2012) found multiple oscillations after the MI of a negative impulse in a northward IMF condition. In the present case, it was possible to unambiguously identify only one oscillation after the maximum deviation. Although a few stations indicate the presence of a second oscillation of weak amplitude, this was not seen consistently at all stations. Looking at the magnetic field variations displayed in Figure six of Hori et al. (2012), even the magnetic field variations show no clear second oscillation; however, filtering of the data results in the detection of second and third oscillations.
Figure 12

Scatter plot between the MI and AMD amplitudes. (a) H component. (b) D component (see text for details).

Hemispheric asymmetry

Figure 13 shows the global plot of the MI amplitude in the latitude-longitude frame (the latitudes are geomagnetic and the longitudes are geographic values). The figure clearly shows the differences in the MI amplitudes between the two hemispheres. For a given geomagnetic latitude, the northern hemisphere (which is a summer hemisphere) shows higher values than the southern hemisphere. Mere magnetopause currents cannot explain the enhancement in the summer hemisphere, and hence it may indicate a contribution due to the enhanced ionospheric conductivities. This observation is in agreement with the findings of Yumoto et al. (1996), who examined hemispheric differences in the MI amplitude of positive impulses at middle and low latitudes. They attributed these observed hemispheric differences to enhanced twin-vortex type ionospheric currents in the summer hemisphere. Therefore, our observations of the hemispheric asymmetry substantiate the role of ionospheric currents in the MI amplitude.
Figure 13

Variation of the MI amplitude on a latitude-longitude frame. The color code shows the magnitude of the MI amplitude, and the geomagnetic equator is shown by a thick horizontal line.

Conclusions

This paper investigates the geomagnetic field responses to a negative pressure impulse of moderate amplitude, which can be useful for the understanding of existing theories. The geomagnetic field response to the negative pressure impulse essentially produces a negative MI in the horizontal component of the geomagnetic field, which is sometimes preceded by a strong positive PRI (Araki and Nagano 1988). Careful inspection of the geomagnetic field response at 97 ground observatories during the presently studied SI event reveals that not a single ground station showed a clear intense positive variation before the MI. Some of the stations showed a very small positive variation before the MI, but the higher resolution data of 1-s sampling interval did not show any enhanced rapid positive variation, and hence we could not clearly identify the PRI signature for the studied event. According to present understanding, the PRI is due to the DPpi system, which is produced by the polarization electric field associated with the shock, mapped to high latitudes (Vestine and Kern 1962; Tamao 1964; Araki 1994). During the present SI case, the velocity of the solar wind changed only by approximately 10 km/s, and no shock was evident; therefore, the absence of a PRI signature during the present case can be justified.

The magnetospheric response to the present SI case recorded by GOES is a clear MI type, the amplitude of the MI increases during daytime, and the ratio of the MI amplitude at a geosynchronous height to that at the ground in the near-dawn sector is less than 1, which is consistent with Kokubun (1983). The MI duration is found to be longer at the ground than at a geosynchronous height, and this could be attributed to the larger distance of the SI source from the ground (the compressional wave requires a longer time to cross a larger path in the magnetosphere to reach the ground). In addition to this, due to inertia of the Earth's environment, the magnetosphere and ionosphere require extra time to reconfigure in response to applied sudden changes (Bhaskar and Vichare 2013). For ground observations, the magnetospheric and ionospheric reconfiguration times contribute to the observed MI duration, while at the altitude of GOES, only the magnetospheric reconfiguration time contributes. Also, as suggested by Nishida (1966), a broadening of the wavefront while passing from a geosynchronous height to the ground could be the cause of the observed longer duration of the MI.

The amplitude of the MI is found to vary with the MLT. In the geomagnetic latitude range between 60°S and 65°N, the MI amplitude is largest in the afternoon to post-dusk and smallest near dawn, except in the equatorial region. The MI of sudden impulse contains contributions from the Chapman-Ferraro currents flowing at the magnetopause, the ionospheric Hall and Pedersen currents, and FACs. The contribution from the magnetopause current is symmetrical about noon (Figure 8b) and hence has the same magnitude and direction in the morning and afternoon. The contributions from FACs are also symmetrical about local noon, flipping direction between local day and night (Araki et al. 2006; Shinbori et al. 2009), and therefore the morning and afternoon sectors would not experience any difference in the MI amplitude due to FACs. Moreover, contributions due to the Pedersen currents are in the opposite direction to those of the FACs during the daytime (Shinbori et al. 2009), and hence the net contribution from these two current systems would be very small during the daytime. We also estimated the contribution due to sudden northward turning of the IMF during the present SI impulse and found this to be very small (approximately −2 nT) at low latitudes. In order to understand the source of the dawn-dusk asymmetry observed in the MI amplitude, we estimated the contribution from the magnetopause currents in the magnetic field recorded by the ground observatories using the Tsyganenko model (T01) and subtracted this value from the observed MI amplitude to obtain the ionospheric contribution in the MI signature. We found that the magnetic field signature due to the ionospheric currents has large negative amplitudes in the afternoon-to-dusk sector and very small negative (or sometimes positive) variations near dawn. This indicates that the ionospheric contribution near dusk is in the same direction as that due to the Chapman-Ferraro current and that the variations are in the opposite directions near dawn. This hypothesis is further substantiated by plotting the equivalent current system derived using H and D components of the residual field, which reveals a two-cell ionospheric current system where the direction of the current appears to be counterclockwise in the morning sector and clockwise in the afternoon sector. The explanation for the existence of this twin-cell ionospheric current system is given below.

Due to the impact of the solar plasma, the convection electric field is set up in the magnetosphere and is transmitted to the polar ionosphere along the magnetic lines of force (Araki 1994). According to Araki and Nagano (1988), during the MI of the negative impulse, the FACs flow into the auroral ionosphere at dusk and out of the ionosphere near dawn, in response to the dusk-to-dawn electric field. The Hall currents generated by the FACs set up twin-vortex current loops at ionospheric heights, each centering near dawn and dusk. The downward FAC sets up a clockwise current vortex, and the upward FAC creates a counterclockwise vortex in the ionosphere, which would result in a positive variation in the horizontal component of the magnetic field near-dawn, on ground (between the center of the current loop and the equator), and a negative variation near dusk. Therefore, the magnetic field due to the twin-cell ionospheric current at near dusk would add to that due to the magnetopause currents and would cause an enhancement of the MI amplitude. Similarly, it would result in the reduction of the MI amplitude in the near dawn. It is possible that the effect of the twin-vortex type ionospheric current generated by the FAC (DP2 Hall currents) extends towards the low-to-mid latitudes (Kikuchi et al. 2001; Araki et al. 2006). However, its magnitude decreases with decreasing latitude, and hence the shape and amplitude of the H waveform are strongly dependent on the latitude and local time. Thus, the observations presented in this paper indicate that the contribution to the MI amplitude observed on the ground due to the ionospheric two-cell convection (DP2) currents driven by the FACs is significant, even for the moderate amplitude SI, and confirms the existence of a dusk-to-dawn electric field during the MI of the negative solar pressure impulse. Furthermore, we have shown that the amplitude of the MI depicts hemispheric asymmetry with higher values in the summer hemisphere than in the winter hemisphere, which once again prove the importance of the ionospheric conductivity and hence the contribution from ionospheric currents in the MI amplitude.

Figure 14 schematically illustrates the dawn-dusk asymmetry through the superimposed magnetic field contributions. As mentioned earlier, no significant shock was evident during the present case of SI, and hence no transient DPpi system was expected. However, if a shock interaction with the magnetosphere occurred, then it would be manifested as the generation of a transient DPpi current system. Therefore, for a general representation of the current system, we have shown the variation due to the DPpi (dotted) in the sketch; however, to be consistent with the present case, this variation is shown to be very small compared to that due to the DPmi (dashed). Magnetic field variations due to the magnetopause currents (DL) are also shown, and the total field due to these superimposed systems is shown by solid curves in the morning (left) and afternoon (right) sectors. We have marked points h1, h2, and h3 in the total field in a similar way to those marked in Figure 4 (note that there is no h3 point in the morning sector). The actual observations depicted in Figures 3 and 4 are fairly consistent with the waveforms sketched here. The waveform of the net total field shows a decrease in the magnetic field after the onset in both the LT sectors, but the shape of the waveform is different. In the morning sector, the net decrease is not smooth, and it takes a longer time to reach the maximum deviation. In the afternoon sector, the MI time duration is shorter than in the morning sector (note the time duration between points h1 and h2) and this is, to some extent, consistent with the observation depicted in Figure 10. During afternoon hours, the magnetic field shows a variation after the peak negative value, which is not seen in the morning hours. The amplitude of the AMD (the variation between points h2 and h3) depends on the strength of the DPmi. Thus, the amplitudes of both the MI and the AMD are controlled by the DPmi variations in the afternoon sector, while in the morning sector there is no AMD variation.Note that in Figure 14, we have ignored the contribution from FACs and Pedersen currents because they are opposite to each other and can therefore be cancelled out, or they deliver only a very small contribution which can either increase or decrease the MI amplitude during the whole day, and therefore there would not be any amplitude differences between the morning and afternoon sectors due to these currents. The amplitude of the MI is shown by the vertical arrow in Figure 14, and it demonstrates a smaller amplitude in the morning and a larger one in the afternoon sector. Thus, the effects of the twin-vortex type ionospheric currents (DPmi) result in larger MI amplitudes in the near-dusk sector and smaller MI amplitudes in the near-dawn sector.
Figure 14

Schematic illustration of geomagnetic response to negative pressure impulse on ground.

A comparison of the MI amplitude at two near-equatorial stations located near-dawn and near-dusk reveals a larger MI amplitude at the near-dawn station, HUA (in the American sector), than at the near-dusk station, TIR (in the Indian sector). If it is assumed that the effect of twin current loops can extend even at equatorial latitudes, then near dawn, the effect should be opposite to that due to the MI and result in a reduction of the amplitude. However, present observations do not appear to be consistent with this supposition.

An interesting feature noticed is that the variation in the magnetic field after the MI shows a very good anti-correlation with the MI amplitudes in both the H and D components. Since at a given station, MI and AMD experience the same ionospheric conductivity, it can be considered that the same enhancing factor is acting on these two variations, and therefore the proportionality exist between the two. In addition, the superimposed magnetic field variations depicted in Figure 14 show variations after the maximum deflection, particularly in the afternoon sector. Thus, the AMD variations are part of the SI variations and can provide information about the DPmi system. The amplitude of the AMD depends on the strength of the DPmi, the time of onset of the DPmi system, the duration of the DPmi, and the strength and duration of DL. In the near future, we plan to study the LT and latitudinal dependence of this variation, which would assist in understanding the DL and DPmi systems more precisely. Very recently, a few studies have investigated the ionospheric flow patterns after the occurrence of an MI. The multiple undulating structures in ionospheric flow variations and in ground magnetic variations have been noted through observational and simulation studies (Yu and Ridley 2011; Hori et al. 2012; Fujita et al. 2012). Several mechanisms (such as the flow vortex chain in the magnetopause region due to the rebound of the magnetopause, multiple ionospheric convection, and compressional wave bouncing between the ionosphere and the dayside magnetopause) have been sought to explain these oscillations. However, it is not possible to gain a clear picture until further observational studies have been performed.

Author's information

The first author is previously known as Geeta Jadhav.

Declarations

Acknowledgements

We express our sincere thanks to Professor T. Araki for important discussions. The results presented in this paper rely on the data collected at magnetic observatories. We therefore thank the national institutes that support the observatories and INTERMAGNET for promoting high standards of magnetic observatory practice (http://www.intermagnet.org). We would also like to give special thanks to the observatories providing 1-s data, ACE Science Center, GOES satellite data center, and WDC-C2, Kyoto, for providing the data.

Authors’ Affiliations

(1)
Indian Institute of Geomagnetism, Navi Mumbai, India

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© Vichare et al.; licensee Springer. 2014

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