Properties of outer solar system pebbles during planetesimal formation from meteor observations
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| Format: | Preprint |
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2024
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| author | Jenniskens, Peter Estrada, Paul R. Pilorz, Stuart Gural, Peter S. Samuels, Dave Rau, Steve Abbott, Timothy M. C. Albers, Jim Austin, Scott Avner, Dan Baggaley, Jack W. Beck, Tim Blomquist, Solvay Boyukata, Mustafa Breukers, Martin Cooney, Walt Cooper, Tim De Cicco, Marcelo Devillepoix, Hadrien Egland, Eric Fahl, Elize Gialluca, Megan Grigsby, Bryant Hanke, Toni Harris, Barbara Heathcote, Steve Hemmelgarn, Samantha Howell, Andy Jehin, Emmanuel Johannink, Carl Juneau, Luke Kisvarsanyi, Erika Mey, Philip Moskovitz, Nick Odeh, Mohammad Rachford, Brian Rollinson, David Scott, James M. Towner, Martin C. Unsalan, Ozan van Wyk, Rynault Wood, Jeff Wray, James D. Pavao, C. Lauretta, Dante S. |
| author_facet | Jenniskens, Peter Estrada, Paul R. Pilorz, Stuart Gural, Peter S. Samuels, Dave Rau, Steve Abbott, Timothy M. C. Albers, Jim Austin, Scott Avner, Dan Baggaley, Jack W. Beck, Tim Blomquist, Solvay Boyukata, Mustafa Breukers, Martin Cooney, Walt Cooper, Tim De Cicco, Marcelo Devillepoix, Hadrien Egland, Eric Fahl, Elize Gialluca, Megan Grigsby, Bryant Hanke, Toni Harris, Barbara Heathcote, Steve Hemmelgarn, Samantha Howell, Andy Jehin, Emmanuel Johannink, Carl Juneau, Luke Kisvarsanyi, Erika Mey, Philip Moskovitz, Nick Odeh, Mohammad Rachford, Brian Rollinson, David Scott, James M. Towner, Martin C. Unsalan, Ozan van Wyk, Rynault Wood, Jeff Wray, James D. Pavao, C. Lauretta, Dante S. |
| contents | In the late stages of accretion leading up to the formation of planetesimals, particles grew to pebbles the size of 1-mm to tens of cm. That is the same size range that dominates the present-day comet mass loss. Meteoroids that size cause visible meteors on Earth. Here, we hypothesize that the size distribution and the physical and chemical properties of young meteoroid streams still contain information about the conditions in the solar nebula during these late stages of accretion. From observations of 47 young meteor showers, we find that freshly ejected meteoroids from long-period comets tend to have low bulk density and are distributed with equal surface area per log-mass interval (magnitude distribution index chi ~ 1.85), suggesting gentle accretion conditions. Jupiter-family comets, on the other hand, mostly produce meteoroids twice as dense and distributed with a steeper chi ~ 2.15 or even chi ~ 2.5, which implies that those pebbles grew from particles fragmenting in a collisional cascade or by catastrophic collisions, respectively. Both comet populations contain an admixture of compact materials that are sometimes sodium-poor, but Jupiter-family comets show a higher percentage (~8% on average) than long-period comet showers (~4%), and a wider range. While there are exceptions in both groups, the implication is that most long-period comets formed under gentle particle growth conditions, possibly near the 30 AU edge of the Trans Neptunian Disk, while most Jupiter family comets formed closer to the Sun where pebbles reached or passed the fragmentation barrier. This is possible if the Scattered Disk represents all objects scattered by Neptune during its migration, while the present-day outer Oort cloud formed only during and after the Sun had moved away from sibling stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_11945 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Properties of outer solar system pebbles during planetesimal formation from meteor observations Jenniskens, Peter Estrada, Paul R. Pilorz, Stuart Gural, Peter S. Samuels, Dave Rau, Steve Abbott, Timothy M. C. Albers, Jim Austin, Scott Avner, Dan Baggaley, Jack W. Beck, Tim Blomquist, Solvay Boyukata, Mustafa Breukers, Martin Cooney, Walt Cooper, Tim De Cicco, Marcelo Devillepoix, Hadrien Egland, Eric Fahl, Elize Gialluca, Megan Grigsby, Bryant Hanke, Toni Harris, Barbara Heathcote, Steve Hemmelgarn, Samantha Howell, Andy Jehin, Emmanuel Johannink, Carl Juneau, Luke Kisvarsanyi, Erika Mey, Philip Moskovitz, Nick Odeh, Mohammad Rachford, Brian Rollinson, David Scott, James M. Towner, Martin C. Unsalan, Ozan van Wyk, Rynault Wood, Jeff Wray, James D. Pavao, C. Lauretta, Dante S. Earth and Planetary Astrophysics 85 In the late stages of accretion leading up to the formation of planetesimals, particles grew to pebbles the size of 1-mm to tens of cm. That is the same size range that dominates the present-day comet mass loss. Meteoroids that size cause visible meteors on Earth. Here, we hypothesize that the size distribution and the physical and chemical properties of young meteoroid streams still contain information about the conditions in the solar nebula during these late stages of accretion. From observations of 47 young meteor showers, we find that freshly ejected meteoroids from long-period comets tend to have low bulk density and are distributed with equal surface area per log-mass interval (magnitude distribution index chi ~ 1.85), suggesting gentle accretion conditions. Jupiter-family comets, on the other hand, mostly produce meteoroids twice as dense and distributed with a steeper chi ~ 2.15 or even chi ~ 2.5, which implies that those pebbles grew from particles fragmenting in a collisional cascade or by catastrophic collisions, respectively. Both comet populations contain an admixture of compact materials that are sometimes sodium-poor, but Jupiter-family comets show a higher percentage (~8% on average) than long-period comet showers (~4%), and a wider range. While there are exceptions in both groups, the implication is that most long-period comets formed under gentle particle growth conditions, possibly near the 30 AU edge of the Trans Neptunian Disk, while most Jupiter family comets formed closer to the Sun where pebbles reached or passed the fragmentation barrier. This is possible if the Scattered Disk represents all objects scattered by Neptune during its migration, while the present-day outer Oort cloud formed only during and after the Sun had moved away from sibling stars. |
| title | Properties of outer solar system pebbles during planetesimal formation from meteor observations |
| topic | Earth and Planetary Astrophysics 85 |
| url | https://arxiv.org/abs/2408.11945 |