Five-planet Nice model

The five-planet Nice model is a recent variation of the Nice model that begins with five giant planets, the current four plus an additional ice giant, in a chain of mean-motion resonances. After the resonance chain is broken, the five giant planets undergo a period of planetesimal-driven migration, followed by a gravitational instability similar to that in the original Nice model. During the instability the additional giant planet is scattered inward onto a Jupiter-crossing orbit and is ejected from the Solar System following an encounter with Jupiter. An early Solar System with five giant planets was proposed in 2011 after numerical models indicated that this is more likely to reproduce the current Solar System.[1]

Background

Current theories of planetary formation do not allow for the accretion of Uranus and Neptune in their present positions.[2] The protoplanetary disk was too diffuse and the time scales too long[3] for them to form before the gas disk dissipated and numerical models indicate that later accretion would be halted once Pluto-sized planetesimals formed.[4]

It is now widely accepted that the Solar System was initially more compact and that the outer planets migrated outward to their current positions.[5] The planetesimal-driven migration of the outer planets was first described, in 1984, by Fernandez and Ip.[6] This process is driven by the exchange of angular momentum between the planets and planetesimals originating from an outer disk.[7] Early dynamical models assumed that this migration was smooth. In addition to reproducing the current positions of the outer planets,[8] these models offered explanations for: the populations of resonant objects,[9] the eccentricity of Pluto's orbit,[10] the inclinations of the hot classical objects and the retention of a scattered disk,[11] and the mass depletion of and the location of the outer edge of the Kuiper belt near the 2:1 resonance with Neptune.[12] However, these models failed to reproduce the eccentricities of the outer planets, leaving them with very small eccentricities at the end of the migration.[13]

The original Nice model resolved this problem by beginning with the Jupiter and Saturn inside their 2:1 resonance. Jupiter's and Saturn's eccentricities are excited when, after a period of slow divergent migration, they cross the 2:1 resonance. This destabilizes the outer Solar System and a series of gravitational encounters ensues during which Uranus and Neptune are scattered outward into the planetesimal disk. There they scatter a great number of planetesimals inward accelerating the migration of the planets. The scattering of planetesimals and the sweeping of resonances through the asteroid belt produce a bombardment of the inner planets. In addition to reproducing the positions and eccentricities of the outer planets,[14] the original Nice model provided for the origin of: the Jupiter[15] and Neptune trojans;[16] the irregular satellites of Saturn, Uranus, and Neptune;[17] the various populations of trans-Neptunian objects;[18] the magnitude of, and with the right initial conditions, the timing of the Late Heavy Bombardment.[19]

The original Nice model was not without its own problems, however. During Jupiter's and Saturn's divergent migration secular resonances sweep through the inner Solar System. As the ν5 secular resonance sweeps through the terrestrial planet region it excites eccentricities beyond their current values potentially destabilizing the inner Solar System.[20] Jupiter's and Saturn's slow approach to the 2:1 resonance is particularly problematic as in numerical simulations Mars's orbit intersects those of the other planets resulting in collisions between planets or in Mars's ejection from the Solar System.[21] The orbits of the asteroids are also significantly altered: the ν16 secular resonance excites inclinations and the ν6 secular resonance excites eccentricities removing low-inclination asteroids as they sweep across the asteroid belt. As a result, the surviving asteroid belt is left with a larger fraction of high inclination objects than is currently observed.[22]

Maintaining the low eccentricities of the terrestrial planets and reproducing the eccentricities and inclinations of the asteroid belt requires a giant planet migration more rapid than that produced in models of planetesimal-driven migration.[22] As a solution to this problem, theorists propose that the divergent migration of Jupiter and Saturn was dominated by planet–planet scattering. Specifically, one of the ice giants was scattered inward onto a Jupiter-crossing orbit by a gravitational encounter with Saturn, after which it was scattered outward by a gravitational encounter with Jupiter.[21] As a result, Jupiter's and Saturn's orbits rapidly diverged. This evolution of the orbits of the giant planets, similar to processes described by exoplanet researchers, is referred to as the jumping-Jupiter scenario.[23]

Ejected planet

The encounters between the ice giant and Jupiter in the jumping-Jupiter scenario often lead to the ejection of the ice giant. For this ice giant to be retained its eccentricity must be damped by dynamical friction with the planetesimal disk, raising its perihelion beyond Saturn's orbit. The planetesimal disk masses typically used in the Nice model are often insufficient for this, leaving system beginning with four giant planets with only three at the end of the instability. The ejection of the ice giant can be avoided if the disk mass is larger, but the separation of Jupiter and Saturn often grows too large and their eccentricities become too small as the larger disk is cleared. These problems led David Nesvorný of the Southwest Research Institute to propose that the Solar System began with five giant planets, with an additional Neptune-mass planet between Saturn and Uranus.[1] Using thousands of simulations with a variety of initial conditions he found that the simulations beginning with five giant planets were ten times more likely to reproduce the current Solar System.[24] A significant migration of Neptune into the planetesimal disk before planetary encounters begin may also be required to preserve the eccentricity of Jupiter. This migration allows a significant fraction of the disk to be removed reducing the dampening of Jupiter's eccentricity after it ejects the ice giant.[25]

Four- and five-giant-planet systems were also investigated by Konstantin Batygin, Michael E. Brown, and Hayden Betts. They found four- or five-planets systems had a similar likelihood of reproducing the orbits of the outer planets, including the oscillations of Jupiter's and Saturn's eccentricities, while preserving a primordial cold classical belt.[26] The low eccentricities of the classical belt were best preserved if the fifth planet was ejected in 10,000 years. Later research, however, reveals that these low eccentricities may by due to the later slow sweeping of mean-motion resonances that removed the higher-eccentricity objects.[27]

A five-planet Nice model

During the early Solar System the five giant planets are captured into a series of mean-motion resonances due to gas-driven migration.[1] A disk of planetesimals orbits beyond these planets, extending to 30 AU. The planetesimal disk is stirred by gravitational interactions with Pluto-massed objects exciting eccentricities and inclinations. After several hundred million years these interactions cause the resonance chain of the giant planets to be broken.[28] The planets then begin to migrate, driven by transfers of angular momentum as they scatter planetesimals. A net inward transfer of planetesimals causes Neptune to migrate outward as most planetesimals it scatters outward return to be scattered again while some of the planetesimals it scatters inward encounter Uranus and are prevented from returning. A similar process occurs for Uranus, the extra ice giant, and Saturn resulting in their outward migration and a transfer of planetesimals inward from the outer belt to Jupiter. Jupiter, in contrast, ejects most of the planetesimals from the Solar System, and as a result migrates inward.[14] Neptune migrates outward several AU and the orbits of the other planets diverge during this planetesimal-driven migration.[29] The divergent migration of the planets leads to resonance crossings, exciting the eccentricities of the planets and destabilizing the planetary system.[25] During this instability the extra ice giant enters a Saturn-crossing orbit and is scattered inward by Saturn onto a Jupiter-crossing orbit. Repeated gravitational encounters with the ice giant drive a step-wise separation of Jupiter and Saturn's orbits leading to a rapid increase of their period ratio until it is greater than 2.3.[21] The ice giant also encounters Uranus and Neptune and crosses parts of the asteroid belt as these encounters increase the eccentricity and semi-major axis of its orbit.[30] After 10,000–100,000 years, the ice giant is ejected from the Solar System following an encounter with Jupiter, making it a rogue planet. The remaining planets then continue to migrate at a declining rate and slowly approach their final orbits as most of the remaining planetesimal disk is removed.

The migrations of the giant planets have many impact throughout the Solar System. The planetesimals scattered inward by Neptune enter planet-crossing orbits, initiating the Late Heavy Bombardment. Some of these planetesimals are captured as Jupiter trojans during encounters between Jupiter and the ejected ice giant as Jupiter's semi-major axis changes.[31] Others are captured as irregular satellites of the giant planets via three body interactions during encounters between the ejected ice giant and the other planets.[32] These encounters can also disturb the orbits of the regular satellites and may be responsible for the inclination of Iapetus's orbit.[33] Saturn's rotational axis is tilted when it slowly crosses a spin-orbit resonance with Neptune.[34][35] While Neptune migrates outward several AU, the hot classical Kuiper disk is formed as some planetesimals orbiting beyond Neptune are captured in resonances, undergo an exchange of eccentricity vs inclination via the Kozai mechanism, and are released onto higher perihelion, stable orbits.[29] Planetesimals captured in Neptune's 2:1 resonance during this early migration are released when an encounter with the ice giant causes its semi-major axis to jump outward, leaving behind a group of low-inclination, low-eccentricity objects with semi-major axes near 44 AU.[36] In the inner Solar System, the rapid separation of the orbits of Jupiter and Saturn reduces the excitation of the eccentricities of the inner planets due to resonance sweeping.[37] Modest changes in the asteroids orbits also occur, possibly shifting the distribution of eccentricities from that of the Grand Tack model toward the current distribution.[30] Asteroid collisional families can also be dispersed as the ice giant crosses the asteroid belt.[38] When the planets reach their present position the innermost part of the asteroid belt is disrupted leading to an extended Late Heavy Bombardment of the inner planets by rocky objects.[39]

Mooted names

According to Nesvorný, colleagues have suggested several names for the hypothetical fifth ice giant—Hades, after the Greek god of the underworld; Liber, after the Roman god of wine and a cognate of Dionysus and Bacchus; and Mephitis, after the Roman goddess of toxic gases. Another suggestion is "Thing 1" from Dr. Seuss's Cat in the Hat children's book.[40]

Notes on Planet Nine

In January 2016, Batygin and Brown proposed that a distant massive ninth planet is responsible for the alignment of the perihelia of several trans-Neptunian objects with semi-major axes greater than 250 AU.[41] Although the mechanism for the ejection of the fifth giant planet in the five-planet Nice model is reminiscent of the origin of Planet Nine, with a gravitational instability including an encounter with Jupiter, it is unlikely to be the same planet. The estimated timing of the capture of Planet Nine onto its distant orbit, three to ten million years after the formation of the Solar System, when the Sun was still in its birth cluster, is inconsistent with a giant-planet instability that was responsible for the Late Heavy Bombardment.[42] A nearby star close enough to aid in Planet Nine's capture would also result in the capture of the Oort cloud objects on orbits much closer than has been estimated from the orbits of comets.[43]

References

  1. 1 2 3 Nesvorný, David (2011). "Young Solar System's Fifth Giant Planet?" (PDF). The Astrophysical Journal Letters 742 (2): L22. arXiv:1109.2949. Bibcode:2011ApJ...742L..22N. doi:10.1088/2041-8205/742/2/L22.
  2. ↑ Levison, Harold F.; Stewart, Glen R. (2001). "Remarks on Modeling the Formation of Uranus and Neptune". Icarus 153 (1): 224–228. Bibcode:2001Icar..153..224L. doi:10.1006/icar.2001.6672.
  3. ↑ Thommes, E. W.; Duncan, M. J.; Levison, Harold F. (2002). "The Formation of Uranus and Neptune among Jupiter and Saturn" (PDF). The Astronomical Journal 123 (5): 2862–2883. arXiv:astro-ph/0111290. Bibcode:2002AJ....123.2862T. doi:10.1086/339975.
  4. ↑ Kenyon, Scott J.; Bromley, Benjamin C. (2008). "Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 Msolar Main-Sequence Stars" (PDF). The Astrophysical Journal Supplement Series 179 (2): 451–483. arXiv:0807.1134. Bibcode:2008ApJS..179..451K. doi:10.1086/591794.
  5. ↑ Levison, Harold F.; Morbidelli, Alessandro (2005). "Interaction of planetesimals with the giant planets and the shaping of the trans-Neptunian belt". Dynamics of Populations of Planetary Systems, Proceedings of IAU Colloquium #197 2004: 303–316. Bibcode:2005dpps.conf..303L. doi:10.1017/S1743921304008798.
  6. ↑ Fernandez, J. A.; Ip, W. H. (1984). "Some dynamical aspects of the accretion of Uranus and Neptune - The exchange of orbital angular momentum with planetesimals". Icarus 58 (1): 109–120. Bibcode:1984Icar...58..109F. doi:10.1016/0019-1035(84)90101-5.
  7. ↑ Levison, Harold F.; Morbidelli, Alessandro; Gomes, Rodney S.; Backman, D. (2007). "Planet Migration in Planetesimal Disks". Protostars and Planets V. B. Reipurth, D. Jewitt, and K. Keil (eds.), University of Arizona Press: 669–684.
  8. ↑ Gomes, Rodney S.; Morbidelli, Alessandro; Levison, Harold F. (2004). "Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?". Icarus 170 (2): 492–507. Bibcode:2004Icar..170..492G. doi:10.1016/j.icarus.2004.03.011.
  9. ↑ Hahn, Joseph M.; Malhotra, Renu (1999). "Orbital Evolution of Planets Embedded in a Planetesimal Disk" (PDF). The Astronomical Journal 117 (6): 3041–3053. arXiv:astro-ph/9902370. Bibcode:1999AJ....117.3041H. doi:10.1086/300891.
  10. ↑ Malhotra, Renu (1995). "The Origin of Pluto's Orbit: Implications for the Solar System Beyond Neptune" (PDF). Astronomical Journal 110: 420. arXiv:astro-ph/9504036. Bibcode:1995AJ....110..420M. doi:10.1086/117532.
  11. ↑ Gomes, Rodney S. (2003). "The origin of the Kuiper Belt high-inclination population". Icarus 161 (2): 404–418. Bibcode:2003Icar..161..404G. doi:10.1016/S0019-1035(02)00056-8.
  12. ↑ Levison, Harold F.; Morbidelli, Alessandro (2003). "The formation of the Kuiper belt by the outward transport of bodies during Neptune's migration". Nature 426 (6965): 419–421. Bibcode:2003Natur.426..419L. doi:10.1038/nature02120. PMID 14647375.
  13. ↑ Morbidelli, Alessandro; Brasser, Ramon; Tsiganis, Kleomenis; Gomes, Rodney S.; Levison, Harold F. (2006). "Constructing the secular architecture of the solar system. I. The giant planets" (PDF). Astronomy and Astrophysics 507 (2): 1041–1052. Bibcode:2009A&A...507.1041M. doi:10.1051/0004-6361/200912876.
  14. 1 2 Tsiganis, Kleomenis; Gomes, Rodney S.; Morbidelli, Alessandro; Levison, Harold F. (205). "Origin of the orbital architecture of the giant planets of the Solar System". Nature 435 (7041): 459–461. Bibcode:2005Natur.435..459T. doi:10.1038/nature03539. PMID 15917800.
  15. ↑ Morbidelli, Alessandro; Levison, Harold F.; Tsiganis, Kleomenis; Gomes, Rodney S. (2005). "Chaotic capture of Jupiter's Trojan asteroids in the early Solar System". Nature 435 (7041): 462–465. Bibcode:2005Natur.435..462M. doi:10.1038/nature03540. PMID 15917801.
  16. ↑ Nesvorný, David; Vokrouhlický, David (2009). "Chaotic Capture of Neptune Trojans". The Astronomical Journal 137 (6): 5003–5011. Bibcode:2009AJ....137.5003N. doi:10.1088/0004-6256/137/6/5003.
  17. ↑ Nesvorný, David; Vokrouhlický, David; Morbidelli, Alessandro (2007). "Capture of Irregular Satellites during Planetary Encounters". The Astronomical Journal 133 (5): 1962–1976. Bibcode:2007AJ....133.1962N. doi:10.1086/512850.
  18. ↑ Levison, Harold F.; Morbidelli, Alessandro; Van Laerhoven, Christa; Gomes, Rodney S.; Tsiganis, Kleomenis (2008). "Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune" (PDF). Icarus 196 (1): 258–273. arXiv:0712.0553. Bibcode:2008Icar..196..258L. doi:10.1016/j.icarus.2007.11.035.
  19. ↑ Gomes, Rodney S.; Levison, Harold F.; Tsiganis, Kleomenis; Morbidelli, Alessandro (2005). "Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets". Nature 435 (7041): 466–469. Bibcode:2005Natur.435..466G. doi:10.1038/nature03676. PMID 15917802.
  20. ↑ Agnor, Craig B.; Lin, D. N. C. (2012). "On the Migration of Jupiter and Saturn: Constraints from Linear Models of Secular Resonant Coupling with the Terrestrial Planets" (PDF). The Astrophysical Journal 745 (2): 143. arXiv:1110.5042. Bibcode:2012ApJ...745..143A. doi:10.1088/0004-637X/745/2/143.
  21. 1 2 3 Brasser, Ramon; Morbidelli, Alessandro; Gomes, Rodney S.; Tsiganis, Kleomenis; Levison, Harold F. (2009). "Constructing the secular architecture of the solar system II: the terrestrial planets" (PDF). Astronomy and Astrophysics 504 (2): 1053–1065. arXiv:0909.1891. Bibcode:2009A&A...507.1053B. doi:10.1051/0004-6361/200912878.
  22. 1 2 Morbidelli, Alessandro; Brasser, Ramon; Gomes, Rodney S.; Levison, Harold F.; Tsiganis, Kleomenis (2010). "Evidence from the Asteroid Belt for a Violent Past Evolution of Jupiter's Orbit" (PDF). The Astronomical Journal 140 (5): 1391–1401. arXiv:1009.1521. Bibcode:2010AJ....140.1391M. doi:10.1088/0004-6256/140/5/1391.
  23. ↑ Fassett, Caleb I.; Minton, David A. (2013). "Impact bombardment of the terrestrial planets and the early history of the Solar System". Nature Geoscience 6 (7): 520–524. Bibcode:2013NatGe...6..520F. doi:10.1038/ngeo1841.
  24. ↑ Stuart, Colin. "Was a giant planet ejected from our solar system?". Physics World. Retrieved 16 January 2014.
  25. 1 2 Nesvorný, David; Morbidelli, Alessandro (2012). "Statistical Study of the Early Solar System's Instability with Four, Five, and Six Giant Planets" (PDF). The Astronomical Journal 144 (4): 17. arXiv:1208.2957. Bibcode:2012AJ....144..117N. doi:10.1088/0004-6256/144/4/117.
  26. ↑ Batygin, Konstantin; Brown, Michael E.; Betts, Hayden (2012). "Instability-driven Dynamical Evolution Model of a Primordially Five-planet Outer Solar System" (PDF). The Astrophysical Journal Letters 744 (1): L3. arXiv:1111.3682. Bibcode:2012ApJ...744L...3B. doi:10.1088/2041-8205/744/1/L3.
  27. ↑ Morbidelli, A.; Gaspar, H. S.; Nesvorny, D., D. (2014). "Origin of the peculiar eccentricity distribution of the inner cold Kuiper belt". Icarus 232: 81–87. arXiv:1312.7536. Bibcode:2014Icar..232...81M. doi:10.1016/j.icarus.2013.12.023.
  28. ↑ Levison, Harold F.; Morbidelli, Alessandro; Tsiganis, Kleomenis; Nesvorný, David; Gomes, Rodney (2011). "Late Orbital Instabilities in the Outer Planets Induced by Interaction with a Self-gravitating Planetesimal Disk" (PDF). The Astronomical Journal 142 (5): 152. Bibcode:2011AJ....142..152L. doi:10.1088/0004-6256/142/5/152.
  29. 1 2 Nesvorný, David. "Evidence for Slow Migration of Neptune from the Inclination Distribution of Kuiper Belt Objects" (PDF). The Astronomical Journal 150 (3): 73. arXiv:1504.06021. Bibcode:2015AJ....150...73N. doi:10.1088/0004-6256/150/3/73.
  30. 1 2 Roig, Fernando; Nesvorný, David (2015). "The Evolution of Asteroids in the Jumping-Jupiter Migration Model". The Astronomical Journal 150 (6): 186. arXiv:1509.06105. Bibcode:2015AJ....150..186R. doi:10.1088/0004-6256/150/6/186.
  31. ↑ Nesvorný, David; Vokrouhlický, David; Morbidelli, Alessandro (2013). "Capture of Trojans by Jumping Jupiter". The Astrophysical Journal 768 (1): 45. arXiv:1303.2900. Bibcode:2013ApJ...768...45N. doi:10.1088/0004-637X/768/1/45.
  32. ↑ Nesvorný, David; Vokrouhlický, David; Deienno, Rogerio. "Capture of Irregular Satellites at Jupiter". The Astrophysical Journal 784 (1): 22. arXiv:1401.0253. Bibcode:2014ApJ...784...22N. doi:10.1088/0004-637X/784/1/22.
  33. ↑ Nesvorný, David; Vokrouhlický, David; Deienno, Rogerio; Walsh, Kevin J. (2014). "Excitation of the Orbital Inclination of Iapetus during Planetary Encounters". The Astronomical Journal 148 (3): 52. arXiv:1406.3600. Bibcode:2014AJ....148...52N. doi:10.1088/0004-6256/148/3/52.
  34. ↑ Vokrouhlický, David; Nesvorný, David (2015). "Tilting Jupiter (a bit) and Saturn (a lot) during Planetary Migration". The Astrophysical Journal 806 (1): 143. arXiv:1505.02938. Bibcode:2015ApJ...806..143V. doi:10.1088/0004-637X/806/1/143.
  35. ↑ Brasser, R.; Lee, Man Hoi (2015). "Tilting Saturn without Tilting Jupiter: Constraints on Giant Planet Migration". The Astronomical Journal 150 (5): 157. arXiv:1509.06834. Bibcode:2015AJ....150..157B. doi:10.1088/0004-6256/150/5/157.
  36. ↑ Nesvorný, David. "Jumping Neptune Can Explain the Kuiper Belt Kernel" (PDF). The Astronomical Journal 150 (3): 68. arXiv:1506.06019. Bibcode:2015AJ....150...68N. doi:10.1088/0004-6256/150/3/68.
  37. ↑ Brasser, R.; Walsh, K. J.; Nesvorny, D. (2013). "Constraining the primordial orbits of the terrestrial planets". Monthly Notices of the Royal Astronomical Society 433 (4): 3417–3427. arXiv:1306.0975. Bibcode:2013MNRAS.433.3417B. doi:10.1093/mnras/stt986.
  38. ↑ Brasil, P. I. O.; Roig, F.; Nesvorný, D.; Carruba, V.; Aljbaae, S.; Huaman, M. E. (2016). "Dynamical dispersal of primordial asteroid families". Icarus 266: 142–151. Bibcode:2016Icar..266..142B. doi:10.1016/j.icarus.2015.11.015.
  39. ↑ Bottke, William F.; Vokrouhlický, David; Minton, David; Nesvorný, David; Morbidelli, Alessandro; Brasser, Ramon; Simonson, Bruce; Levison, Harold F. (2012). "An Archaean heavy bombardment from a destabilized extension of the asteroid belt". Nature 485 (7396): 78–81. Bibcode:2012Natur.485...78B. doi:10.1038/nature10967.
  40. ↑ A New Name for an Old Planet: New Scientist: 01.10.2011: 15, https://www.newscientist.com/article/dn20952-missing-planet-explains-solar-systems-structure/
  41. ↑ Batygin, Konstantin; Brown, Michael E. (20 January 2016). "Evidence for a distant giant planet in the Solar system". The Astronomical Journal 151 (2). arXiv:1601.05438. Bibcode:2016AJ....151...22B. doi:10.3847/0004-6256/151/2/22.
  42. ↑ Drake, Nadia. "How can we find planet nine? (and other burning questions)". No place like home. National Geographic. Retrieved 30 January 2016.
  43. ↑ Raymond, Sean. "Planet Nine: kicked out by the moody young Solar System?". PlanetPlanet. Retrieved 27 February 2016.
This article is issued from Wikipedia - version of the Monday, May 02, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.