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Table 1 Results from the IMEX cometary dust trails simulations for MMX

From: Modelling cometary meteoroid stream traverses of the Martian Moons eXploration (MMX) spacecraft en route to Phobos

Comet

Time interval with flux

Duration

Day with

Maximum

Fluence

Impact speed at maximum flux

Impact direction

 

\(\ge 10^{-3}\mathrm {\,m}^{-2}\mathrm {\,day}^{-1}\)

 

maximum flux

flux

 

\(|v_{\mathrm {imp}}|\)

\(v_x\)

\(v_y\)

\(v_z\)

\(\lambda _{\mathrm {ecl}}\)

\(\beta _{\mathrm {ecl}}\)

  

[days]

 

[\(\mathrm {m}^{-2}\mathrm {\,day}^{-1}\)]

[\(\mathrm {m}^{-2}\)]

[\(\mathrm {km\,s}^{-1}\)]

[\(\mathrm {km\,s}^{-1}\)]

[\(\mathrm {km\,s}^{-1}\)]

[\(\mathrm {km\,s}^{-1}\)]

[\(^{\circ }\)]

[\(^{\circ }\)]

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

(9)

(10)

(11)

(12)

Interplanetary Transfer Phase

21P/Giacobini-Zinner

04.10.2024–11.10.2024

8

05.10.2024

0.0082

0.013

20.2

1.4

0.9

−20.1

212

85

24P/Schaumasse

14.12.2024–16.12.2024

2

16.12.2024

0.0011

0.002

20.4

−5.6

−17.1

9.6

72

−28

45P/H-M-P

05.05.2025–17.05.2025

13

17.05.2025

0.0013

0.015

17.6

−17.4

2.7

0.0

351

0

103P/Hartley

25.10.2024–26.10.2024

2

26.10.2024

0.0009

0.001

10.0

−7.0

1.1

−7.1

351

45

Mars Orbital Phase

3D/Biela

30.05.2026–15.06.2026

17

10.06.2026

0.0064

0.006

20.5

−18.5

−8.0

−3.8

23

11

3D/Biela

13.06.2027–25.06.2027

13

20.06.2027

0.0045

0.050

20.4

−18.5

−7.8

3.6

23

−10

19P/Borrelly

08.09.2026–18.09.2026

11

15.09.2026

0.0310

0.332

15.7

−2.4

−0.3

15.5

8

−81

24P/Schaumasse

02.09.2026–13.09.2026

12

09.09.2026

0.0039

0.041

16.4

−7.6

−13.9

4.1

61

−14

45P/H-M-P

21.12.2027–26.12.2027

6

24.12.2027

0.0355

0.120

22.3

−16.6

15.0

− 0.2

318

1

114P/Wiseman-Skiff

04.10.2026–07.10.2026

3

06.10.2026

0.1535

0.300

11.0

-4.9

−1.1

−9.9

13

63

185P/Petriew

24.06.2026–05.07.2026

12

04.07.2026

0.0046

0.037

10.7

−2.3

3.1

−10.0

306

69

275P/Hermann

22.03.2027–25.03.2027

4

24.03.2027

0.0110

0.034

12.3

−2.6

−5.7

−10.6

66

59

  1. The time interval of the trail traverse together with the predicted maximum flux (of \(100\,\mu \mathrm { m}\) and bigger particles) are given in columns (2) to (5). Column (6) gives the fluence on to a \(1\,\mathrm {m}^{2}\) detector detectable during the time interval given in column (2). Columns (7) to (10) give the speed vector, while columns (11) and (12) give the impact direction of the particles in ecliptic coordinates (opposite to speed vector), both in the spacecraft-centered reference frame. The impact direction corresponds to the radiant of a meteor stream in a planetary atmosphere