- Open Access
Planets in orbit around β Pictoris formed the orbital architecture of planetesimal belts?
© The Society of Geomagnetism and Earth, Planetary and Space Sciences, The Seismological Society of Japan 2010
- Received: 30 July 2008
- Accepted: 11 November 2009
- Published: 7 February 2015
We report near-infrared imaging observations of the β Pic dust disk, from which we infer the orbital architecture of planetesimal belts that remain near mean motion resonances (MMRs) with a planet at 62 AU. Our results reveal that one of the previously identified planetesimal belts lies in the 2/3 MMR with the planet, similar to the resonant relation between Plutinos and Neptune. We suggest that all the previously reported planetesimal belts are located near the 2/3 MMRs of four planets whose spatial arrangements make a similar figure of Jupiter, Saturn, Uranus, and Neptune. This implies that the Solar System is a prototype of planetary systems around main-sequence stars in terms of planets” configuration, as expected from planet formation theories.
- Stars: individual (β Pictoris)
- stars: planetary systems
- planetary systems: formation
- Kuiper Belt
Imaging observations of the A5 V star β Pictoris have revealed its circumstellar dust disk viewed almost edgeon from the Earth (Smith and Terrile, 1984; Paresce and Burrows, 1987; Golimowski et al., 1993, 2006; Kalas and Jewitt, 1995; Tamura et al., 2006). The disk is not primordial, but a dynamical consequence of debris that are continuously replenished by mutual collisions between planetesimals (Weissman, 1984; Backman et al., 1992; Backman and Paresce, 1993; Krivova et al., 2000). The location of the debris or dust is most likely confined near its parentbody planetesimals in nearly coplanar orbits (Krivov et al., 2000; Freistetter et al., 2007). This indicates that the spatial distribution of planetesimals can be traced through observed brightness profiles of the dust disk. A warp and rings in the inner disk suggest that the structures are formed by gravitational influences of planets on the planetesimals (Heap et al., 2000; Wahhaj et al., 2003; Okamoto et al., 2004; Freistetter et al., 2007). Surface brightness along the mid-plane of the β Pic disk shows a kink in its radial profile around 100 AU from the star (Golimowski et al., 1993, 2006; Kalas and Jewitt, 1995; Krivova et al., 2000). Such a brightness profile is consistent with the radial dust distribution that peaks around 100 AU, analogous to the dust in the Kuiper Belt (Backman et al., 1992; Backman and Paresce, 1993). These observations are well modeled under the assumption that planetesimals are concentrated in the range of 80–120 AU (Augereau et al., 2001; Thébault and Augereau, 2005). It is worth noting that, in the solar system, a number of trans-neptunian objects in the Kuiper Belt are trapped in mean motion resonances (MMRs) with Neptune (Luu and Jewitt, 2002). Analogous to the outer edge of the Kuiper Belt at the 1/2 MMR with Neptune, the sharp drop in the surface density of β Pic planetesimals may be linked to the outer edge of a planetesimal belt at the 1/2MMR with a yet unseen planet, which is hereafter referred to as Planet N. Near-infrared observations of linear polarization revealed a dip at 5.3±0.1 arcsec (i.e., 102–104 AU) in the north-east and south-west directions of the β Pic disk (Tamura et al., 2006). We can interpret this dip as a paucity of planetesimals in the region from 1/2 MMR to 4/9 MMR with Planet N. Placing the dip in the middle of the 1/2 and 4/9 MMRs, we would find Planet N at 62 AU from the central star.
Spatially localized enhancements in the K-band brightness of the disk manifested a sign of multiple planetesimal rings (Tamura et al., 2006). If planetesimals in the β Pic system reside in MMRs with a planet, the observed clumps in the surface brightness profile of the disk can be simply resonant structures of planetesimal belts. Therefore, we seek evidence for the presence of Planet N by investigating whether its MMRs match the locations of observed humps in the brightness distribution of the disk.
Using the Subaru 8.2-m telescope and the CIAO infrared coronagraph imager with adaptive optics, we imaged the circumstellar dust disk of β Pic in H (1.65 μm) and K (2.2 μm) bands on January 4, 2003. A detailed description of the observations and the data reduction as well as a preliminary analysis of the K-band data can be found in Tamura et al. (2006). Hereafter, we focus on our data analyses to find observational evidence of multiple planetesimal rings in our data set. Signals of planetesimal rings would appear as brightness peaks in both northeast and southwest directions as well as both H- and K-bands. We compare the excess emission in both bands after subtracting their continuum levels (see Section 3). A weak correlation with a correlation coefficient (r) of 0.3 is indeed found between the clumps in H- and K-bands. We assess the statistical significance of brightness peaks by testing the null hypothesis that the observed brightness distribution is merely random noise superimposed on a smooth curve of radiation scattered by circumstellar dust. Therefore, the random noise is smoothed out by averaging over both wavelengths and offset directions, resulting in a smooth declining curve of the average surface intensity. On the one hand, we admit that fake features might appear in the average brightness, if the random noise was not completely smoothed out by the averaging procedure. On the other hand, even real enhancements in the K-band brightness might be diluted with the H-band brightness, because the latter had a lower signal-to-noise ratio than the former. In such an analysis, only strong peaks, which we attribute to nearly circular, coplanar rings, will remain in the residuals after subtraction of a smooth brightness component. Therefore, we derive the residuals from the mean of the surface intensities to trace possible resonant structures of multiple planetesimal rings associated with Planet N.
We use a dip at 5.3 arcsec in the polarimetric data of Tamura et al. (2006) to infer the location of Planet N as analogous to the outer edge of the Kuiper Belt in the solar system, while the evolutionary history of the β Pic system is likely different from that of the solar system. However, a different evolutional history does not necessarily mean that there is no paucity of planetesimals between the 1/2 and 4/9 MMRs of a planet in the β Pic system. Therefore, we do not argue the presence of the planet at 62 AU from an evolutional point of view, but we hereafter examine it with our observational data. Note that the dip at 5.3 arcsec in our polarimetric data is simply our motivation to seek a planet around 62 AU.
4.1 Large dust particles
The radial distribution of edge-on-disk brightness traces the radial distribution of the dust that dominates the total cross section of light scattering by dust particles in the disk. If the size distribution of the dust in the β Pic disk is similar to that of interplanetary dust in the solar system or that of cometary dust, the scattering cross section is determined by large dust particles (Grün et al., 1985; McDonnell et al., 1987; Kolokolova et al., 2007). Indeed, the infrared spectra of cometary dust and β Pic dust are very much alike (Knacke et al., 1993). Although this does not guarantee the similarity in the size distribution between cometary dust and β Pic dust, we do not find a reason that small dust particles dominate the scattering cross section. Large dust particles tend to scatter stellar radiation in forward directions and to stay near the orbit of their parent bodies (e.g., Kresák,1976; Bohren and Huffman, 1983). Polarimetric observations of the β Pic debris disk have revealed an effect of strong forward scattering that decreases the degree of linear polarization with decreasing radial distance from the star (Krivova et al., 2000; Tamura et al., 2006). The strong forward scattering is also manifested in the pronounced dip around 5.3 arcsec in the radial profile of linear polarization, in contrast to its insignificant correspondence in the radial profile of our K-band intensity (Tamura et al., 2006). Since large dust particles are less affected by stellar radiation pressure, they accumulate along the orbit of their parent body as seen in dust trails of comets (e.g., Ishiguro et al., 2002). In addition, collisional models of debris disks predict that the peak of thermal radiation from dust particles appears at a planetesimal belt in a typical debris disk (Krivov et al., 2008). Even though the location of parent-body planetesimals may not exactly coincide with associated dust rings, the difference is not necessarily notified with our spacial resolution of approximately 4 AU. Therefore, the location of a planetesimal belt can be identified by observations of its associated dust ring, unless the β Pic dust is very different from the dust in the solar system and in typical debris disks. We conclude that observations of stellar radiation scattered by dust particles in a typical debris disk would provide an opportunity of detecting extrasolar planets in the disk if the orbital architecture of planetesimal belts are shaped by the gravitational field of the planets.
4.2 The outermost planet
Even though the radial distribution of planetesimals steeply drops near the 1/2 MMR with Planet N, the β Pic system appears to consist of planetesimal rings on the outskirts of the planetesimal disk beyond the 1/2 MMR. We note that we certainly have to wait for future observations to confirm our identification with these high-order resonances, which could be criticized to be premature at this stage. Hahn and Malhotra (1999) have shown that planetary migration results in concentration of planetesimals at the outermost planet”s exterior MMRs and allows the planetesimals beyond 1/2 MMR to remain in orbits with low eccentricities and low inclinations. The resonant planetesimals beyond Planet N”s 1/2 MMR seem to reside in nearly circular, low-inclination orbits, because they are identified at the same distance from the star along northeast and southwest directions. This may indicate that these outer planetesimal rings around β Pic are relatively undisturbed remnants of the natal planetesimal disk. Although the numerical results by Hahn and Malhotra (1999) might depend on various input parameters, we may expect that Planet N is the outermost planet in the β Pic system.
Owing to its spatially resolved edge-on viewing, the width of the β Pic disk has been measured over a wide range of distances. The disk width increases with distance in the outer disk (>100 AU), but it is almost constant in the inner disk (<100 AU) (Kalas and Jewitt, 1995; Krivova et al., 2000; Golimowski et al., 2006; Tamura et al., 2006). The flared structure of the outer disk is akin to the structure of the outer Kuiper Belt where the planetesimal disk is flared up from the ecliptic plane. Lecavelier des Etangs (1998) pointed out that the vertical structure of the β Pic disk might have resulted from the outward migration of multiple giant planets. In terms of Planet N, planetary migration is consistent with a planet formation scenario that precludes insitu formation of a planet at 62 AU around β Pic (Nakano, 1988). To place a planet at 62 AU around β Pic, however, the planet formation scenario might require rapid planet migration that is at odds with nearly circular, coplanar planetesimal rings. Consequently, the presence of Planet N at 62 AU would give new insights into formation of a planetary system, in particular, planetary migration.
4.3 Planetary system
Mid-infrared images of the inner β Pic disk revealed four inner rings at 14±1 (A ring), 28±3 (B ring), 52±2 (C ring), and 82±2 AU (D ring) with the greatest optical depth in the D ring (Wahhaj et al., 2003). We notice that the location of the D ring corresponds to the 2/3 MMR of planetesimals with Planet N at 81.2 AU. Note that Pluto and Plutinos in the 2/3 MMR with the outermost planet Neptune are known to have stable orbits (Luu and Jewitt, 2002). Therefore, the greatest optical depth of the D ring is reasonably a consequence of the strong 2/3 MMR with Planet N, the outermost planet of the β Pic system. In addition to the A and B rings, mid-infrared spectral features of silicates revealed the presence of a planetesimal belt (O ring) around 6 AU (Okamoto et al., 2004). If the O ring were a main asteroid belt in relation to a yet undetected planet having the A ring in its 2/3 MMR, the hypothetical planet, which is hereafter referred to as Planet J, would exist at 11 AU. In fact, Jupiter-mass Planet J around 10–12 AU in a slightly eccentric orbit is an appropriate solution to generate the warp of the disk and a number of star-grazing comets observed in the β Pic system (Lecavelier des Etangs, 1998; Heap et al., 2000; Freistetter et al., 2007). Located slightly inside Planet J is the ice boundary around 9 AU from the central star. A model of planet formation indicates that gas giants can form slightly outside the ice boundary (Ida and Lin, 2004). Therefore, we expect Planet J, if exists, to be a gas giant1.
The presence of a planetary system around β Pic is consistent with available observations of the β Pic dust disk from near- to mid-infrared wavelengths. The detection of planetesimal rings in the visible wavelength range is more difficult, because a number of clumps in the foreground more easily obscure a planetesimal ring that is tangential to the line of sight. In fact, optical observations with Hubble Space Telescope have not succeeded in imaging the clumps of planetesimals up to date (Golimowski et al., 2006). On the one hand, higher resolution infrared observations are able to reveal the resonant structures of planets and to identify their precise locations. On the other hand, numerical 116 H. KIMURA et al.: PLANETS IN ORBIT AROUND β PICTORIS dynamical simulations of planetesimals in the stellar and planetary gravitational fields allow us to constrain the mass and orbital parameters of the planets. If the presence of Planets J, S, U and N were confirmed by future observations, then the coming question would be: Are there Earthlike planets in the β Pic system? A radial velocity survey excludes the presence of an inner giant planet in the immediate vicinity of the star (≤1 AU) (Galland et al., 2006). However, the result does not contradict the presence of Earth-like planets in orbit around β Pic within a few AU from the star.
When revising the manuscript, Lagrange et al. (2009a, 2009b) reported a probable detection of a giant planet around 8 AU, which is in accord with the location of Planets J within the accuracy of the observational data used in our discussion.
We place 2, 0.5, 0.1, 0.1 Jovian-mass planets to simulate their gravitational influences on planetesimals initially distributed from 5 to 110 AU in a disk according to a power-law radial distribution with the power of -0.5. Our results on the relative abundance of planetesimals do not depend on the assumed distribution of planetesimals, because each test particle in our simulation has no gravitational force on the other particles.
This research is supported by grants from CPS, JSPS, and MEXT Japan.
- Augereau, J. C., R. P. Nelson, A. M. Lagrange, J. C. B. Papaloizou, and D. Mouillet, Dynamical modeling of large scale asymmetries in the \ Pictoris dust disk, Astron. Astrophys., 370, 447–455, 2001.View ArticleGoogle Scholar
- Backman, D. E. and F. Paresce, Main-sequence stars with circumstellar solid material: the Vega phenomenon, in Protostars and Planets III, edited by E. H. Levy and J. I. Lunine, pp. 1253–1304, Univ. Arizona Press, Tucson, 1993.Google Scholar
- Backman, D. E., F. C. Gillett, and F. C. Witteborn, Infrared observations and thermal models of the \ Pictors disk, Astrophys. J., 385, 670–679, 1992.View ArticleGoogle Scholar
- Bohren, C. F. and D. R. Huffman, Absorption and Scattering of Light by Small Particles, Wiley-Interscience, New York, 1983.Google Scholar
- Freistetter, F., A. V. Krivov, and T. Lohne, Planets of \ Pictoris revisited, Astron. Astrophys., 466, 389–393, 2007.View ArticleGoogle Scholar
- Galland, F., A.-M. Lagrange, S. Udry, A. Chelli, F. Pepe, J.-L. Beuzit, and M. Mayor, Extrasolar planets and brown dwarfs around A-F type stars. III. β Pictoris: looking for planets, finding pulsations, Astron. Astrophys., 447, 355–359, 2006.View ArticleGoogle Scholar
- Gaudi, B. S. et al., Discovery of a Jupiter/Saturn analog with gravitational microlensing, Science, 319, 927–930, 2008.View ArticleGoogle Scholar
- Golimowski, D. A., S. T. Durrance, and M. Clampin, Coronagraphic imaging of the \ Pictoris circumstellar disk: Evidence ofchanging disk structure within 100 AU, Astrophys. J., 411, L41–L44, 1993.View ArticleGoogle Scholar
- Golimowski, D. A. et al., Hubble Space Telescope ACS multiband coron-agraphic imaging of the debris disk around \ Pictoris, Astron. J., 131, 3109–3130, 2006.View ArticleGoogle Scholar
- Grün, E., H. A. Zook, H. Fechtig, and R. H. Giese, Collisional balance of the meteoritic complex, Icarus, 62, 244–272, 1985.View ArticleGoogle Scholar
- Hahn, J. M. and R. Malhotra, Orbital evolution of planets embedded in a planetesimal disk, Astron. J., 117, 3041–3053, 1999.View ArticleGoogle Scholar
- Heap, S. R., D. J. Lindler, T. M. Lanz, R. H. Cornett, I. Hubeny, S. P. Martin, and B. Woodgatte, Space telescope imaging spectrograph coronagraphic observations of \ Pictoris, Astrophys. J., 539, 435–444, 2000.View ArticleGoogle Scholar
- Ida, S. and D. N. C. Lin, Toward a deterministric model of planetary formation. I. A desert in the mass and semimajor axis distributions of extrasolar planets, Astrophys. J., 604, 388–413, 2004.View ArticleGoogle Scholar
- Ishiguro, M., J. Watanabe, F. Usui, T. Tanigawa, D. Kinoshita, J. Suzuki, R. Nakamura, M. Ueno, and T. Mukai, First detection of an optical dust trail along the orbit of 22P/Kopff, Astrophys. J., 572, L117–L120, 2002.View ArticleGoogle Scholar
- Kalas, P. and D. Jewitt, Asymmetries in the Beta Pictors dust disk, Astron. J., 110, 794–804, 1995.View ArticleGoogle Scholar
- Knacke, R. F., S. B. Fajardo- Acosta, C. M. Telesco, J. A. Hackwell, D. K. Lynch, and R. W. Russell, The silicates in the disk of \ Pictoris, Astrophys. J., 418, 440–450, 1993.View ArticleGoogle Scholar
- Kokubo, E. and J. Makino, A modified Hermite integrator for planetary dynamics, Publ. Astron. Soc. Jpn., 56, 861–868, 2004.View ArticleGoogle Scholar
- Kolokolova, L., H. Kimura, N. Kiselev, and V. Rosenbush, Two different evolutionary types of comets proved by polarimetric and infrared properties of their dust, Astron. Astrophys., 463, 1189–1196, 2007.View ArticleGoogle Scholar
- Kresák, L., Orbital evolution of the dust streams released from comets, Bull. Astr. Inst. Czechosl., 27, 35–46, 1976.Google Scholar
- Krivov, A. V., I. Mann, and N. A. Krivova, Size distributions of dust in circumstellar debris discs, Astron. Astrophys., 362, 1127–1137, 2000.Google Scholar
- Krivov, A. V., S. Müller, T. Lohne, and H. Mutschke, Collisional and thermal emission models of debris disks: Toward planetesimal population properties, Astrophys. J., 687, 608–622, 2008.View ArticleGoogle Scholar
- Krivova, N. A., A. V. Krivov, and I. Mann, The disk of \ Pictoris in the light of polarimetric data, Astrophys. J., 539, 424–434, 2000.View ArticleGoogle Scholar
- Lagrange, A.-M. et al., A probable giant planet imaged in the \ Pictoris disk. VLT/NaCo deep L’-band imaging, Astron. Astrophys., 493, L21–L25, 2009a.View ArticleGoogle Scholar
- Lagrange, A.-M. et al., Constraining the orbit of the possible companion to \ Pictoris. New deep imaging observations, Astron. Astrophys., 506, 927–934, 2009b.View ArticleGoogle Scholar
- Lecavelier des Etangs, A., Planetary migration and sources of dust in the \ Pictoris disk, Astron. Astrophys., 337, 501–511, 1998.Google Scholar
- Luu, J. X. and D. C. Jewitt, Kuiper Belt Objects: Relics from the accretion disk of the Sun, Ann. Rev. Astron. Astrophys., 40, 63–101, 2002.View ArticleGoogle Scholar
- McDonnell, J. A. M. et al., The dust distribution within the inner coma of comet P/Halley 1982i: encounter by Giotto’s impact detectors, Astron. Astrophys., 187, 719–741, 1987.Google Scholar
- Mouillet, D., A.-M. Lagrange, J.-L. Beuzit, and N. Renaud, A stellar coronagraph for the COME-ON-PLUS adaptive optics system. II. First astronomical results, Astron. Astrophys., 324, 1083–1090, 1997.Google Scholar
- Nakano, T., Formation of planets around stars of various masses II. Stars of two and three solar masses and the origin and evolution ofcircumstellar dust clouds, Mon. Not. Roy. Astron. Soc., 230, 551–571, 1988.View ArticleGoogle Scholar
- Okamoto, Y. K. et al., An early extrasolar planetary system revealed by planetesimal belts in \ Pictoris, Nature, 431, 660–663, 2004.View ArticleGoogle Scholar
- Paresce, F. and C. Burrows, Broad-band imaging of the Beta Pictoris circumstellar disk, Astrophys. J., 319, L23–L25, 1987.View ArticleGoogle Scholar
- Smith, B. A. and R. J. Terrile, A circumstellar disk around \ Pictoris, Science, 226, 1421–1424, 1984.View ArticleGoogle Scholar
- Tamura, M., M. Fukagawa, H. Kimura, T. Yamamoto, H. Suto, and L. Abe, First two-micron imaging polarimetry of \ Pictoris, Astrophys. J., 641, 1172–1177, 2006.View ArticleGoogle Scholar
- Thébault, P. and J.-C. Augereau, Upper limit on the gas density in the \ Pictoris system: The effect of gas drag on dust dynamics, Astron. Astrophys., 437, 141–148, 2005.View ArticleGoogle Scholar
- Thébault, P. and H. Beust, Falling evaporating bodies in the \ Pictoris system. Resonance refilling and long term duration of the phenomenon, Astron. Astrophys., 376, 621–640, 2001.View ArticleGoogle Scholar
- Wahhaj, Z., D. W. Koerner, M. E. Ressler, M. W. Werner, D. E. Backman, and A. I. Sargent, The inner rings of \ Pictoris, Astrophys J., 584, L27–L31, 2003.View ArticleGoogle Scholar
- Weissman, P. R., The Vega particulate shell: comets or asteroids?, Science, 224, 987–989, 1984.View ArticleGoogle Scholar