Our solar system, where planets have a range of sizes and move in near-circular paths, may be rather unusual, according to a German-British team led by Professor Pavel Kroupa of the University of Bonn. The astronomers, who publish their model in the journal Monthly Notices of the Royal Astronomical Society, find that forming planetary systems may be knocked around by crashes with nearby clumps of material, leading to systems where planets have highly inclined orbits and where the smaller (and potentially habitable) worlds are thrown out completely.
The planets in our solar system, including the Earth, orbit in the same direction around the Sun as the Sun spins, mostly move in paths not so different from circles and are also more or less lined up into a plane not tilted very far with respect to the solar equator. But planetary systems around other stars can be very different, with some worlds moving in the opposite direction to the spin of their stars and with highly tilted orbits. For the first time the team of astronomers think they have a convincing model that explains these radically different systems.
Both the shape of and direction of travel of planets in our solar system were thought to result entirely from the formation of the Sun and planets more than 4,600 million years ago. Our local planetary system is believed to have formed as a cloud of gas and dust (a nebula) that collapsed into a rotating disk under the influence of gravity. The planets then grew from clumps of material within this so-called protoplanetary disk.
The new work suggests that oddly shaped orbits may result from a rather less smooth process. The team think that if the protoplanetary disk enters another cloud of material, it can draw off up to about 30 times the mass of Jupiter from the cloud. Adding this extra gas and dust tilts the disk and hence the angle of the final orbits. Most planetary systems are thought to form in clusters of stars, where the member stars are fairly close together, so these encounters may be very common.
Team member Dr. Ingo Thies, also of the University of Bonn, has carried out computer simulations to test the new idea. He finds that as well as tilting over, loading the protoplanetary disk with material can even reverse its spin, so that it turns in a ‘retrograde’ sense, where it rotates in the opposite sense to its parent star. At the same time, the encounter compresses the inner region of the disk, possibly speeding up the planetary formation process.
In those circumstances, the simulation suggests that any planets that form will then be in highly inclined or even retrograde orbits. In some cases the orbits may even be tilted with respect to each other, leading to a highly unstable system. One by one, the least massive planets will be ejected completely, leaving behind a small number of ‘hot Jupiters’, massive worlds that move in orbits extremely close to their star.
In less extreme cases, the disk may only collect a small amount of additional gas and dust and change its tilt by a small amount. This may be what happened in our own solar system, where the weighted average tilt of planetary orbits to the Sun’s equator is about 7 degrees.
Dr. Thies believes the Sun and planets are amongst the more orderly systems. “Like most stars, the Sun formed in a cluster, so probably did encounter another cloud of gas and dust soon after it formed. Fortunately for us, this was a gentle collision, so the effect on the disk that eventually became the planets was relatively benign. If things had been different, an unstable planetary system may have formed around the Sun, the Earth might have been ejected from the solar system and none of us would be here to talk about it.”
Professor Kroupa sees the model as a big step forward. “We may be on the cusp of solving the mystery of why some planetary systems are tilted so much and lack places where life could thrive. The model helps to explain why our solar system looks the way it does, with the Earth in a stable orbit and larger planets further out. Our work should help other scientists refine their search for life elsewhere in the Universe.”
Science Contacts (Team Members):
Dr. Ingo Thies
Argelander-Institut fuer Astronomie (AIfA) Sternwarte
University of Bonn
+49 (0)228 73 3659; cell: +49
ithies@astro.uni-bonn.de
Prof. Pavel Kroupa
Argelander-Institut fuer Astronomie (AIfA) Sternwarte
University of Bonn
+49 (0)228 736 140; cell: +44 (0)177 956 6127
pavel@astro.uni-bonn.de
Dr. Simon P. Goodwin
University of Sheffield
+44 (0)114 22 23585; cell: +44 (0)798 680 1863
s.goodwin@sheffield.ac.uk
Prof. Anthony Whitworth
University of Cardiff
+44 (0)29 208 74798
anthony.whitworth@astro.cf.ac.uk
Dr. Dimitrios Stamatellos
University of Cardiff
+44 (0)29 208 75999
dimitrios.stamatellos@astro.cf.ac.uk
Images & Captions
A collection of 30 Hubble Space Telescope images of protoplanetary disks in the Orion Nebula is available at http://www.spacetelescope.org/news/heic0917/ (Credit: NASA, ESA and L. Ricci (ESO))
A set of 23 images illustrating the new concept are available from the subfolders at http://www.astro.uni-bonn.de/~ithies/images/Planet_Formation_Illustrated/
1. encounter1: The star and protoplanetary disk encounter a dense clump of gas and dust.
2. encounter2: The star and disk capture material from the clump.
3. annulus1: The situation immediately after the disk-clump encounter. Material from the clump is in a tilted ring around the star and disk.
4. annulus2: After 30,000 years the disk and ring are aligned.
5. inclined1: After 100,000 years the disk and ring have merged.
6. inclined2: After a few million years planets start to form in the disk.
7. inclined3: The star is now host to a set of planets in highly tilted orbits.
8. ejection1: There is a gravitational interaction between the smaller and larger planet.
9. ejection2: After the encounter, the smaller planet is ejected from the system and the large planet moves into an eccentric orbit.
10. ejection3: The orbit of the large planet circularizes and shrinks, bringing it closer to its parent star to become a ‘hot Jupiter’.
11. Kozai1: In a different scenario, the two planets again start off in orbits with different tilts.
12. Kozai2: This time the inner planet first moves into an eccentric orbit.
13. Kozai3: Eventually the inner planet has a small circular orbit and has become a ‘hot Jupiter’.
14. formation1: The first of six images describing the conventional model of planet formation, starting with a cloud of gas and dust (like for example the center of the Orion Nebula).
15. formation2: The cloud fragments, with smaller clumps forming under the influence of gravity.
16. formation3: The clumps rotate faster as they contract.
17. formation 4: This then causes the clumps to flatten into a disk.
18. formation 5: In the central region of the clump a protostar forms.
19. formation 6-7: Mass is lost from the disk and the protostar continues to contract and heat up.
20. formation 7: Protoplanets form in the disk.
21. formation 8: A stable planetary system forms, but this model does not explain the tilt observed in most cases.
22. system1: A stable planetary system that resembles our own.
23. system2: A planetary system with highly inclined orbits that may become unstable over time.
(All these images should be credited to I. Thies/University of Bonn)
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The new work is published in “A natural formation scenario for misaligned and short-period eccentric extrasolar planets”, Thies I., Kroupa P., Goodwin S., Stamatellos D. and Whitworth A., Monthly Notices of the Royal Astronomical Society, in press. A preprint of the paper can be seen at http://arxiv.org/abs/1107.2113
The research was funded by Deutsche Forschungsgemeinschaft (DFG) grant KR1635/25 as part of the “Schwerpunktproject” SPP 1385 “The First 10 Million Years of the Solar System — a Planetary Materials Approach”.
The Royal Astronomical Society (RAS, http://www.ras.org.uk), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science. The RAS organizes scientific meetings, publishes international research and review journals, recognizes outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 3,500 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.
