Ice Inheritance in Dynamical Disk Models
The compositions of planet-forming disks are set by a combination of material inherited from the interstellar medium and material reprocessed during disk formation and evolution. Indeed, comets and primitive meteorites exhibit interstellar-like isotopic ratios and/or volatile compositions, supportin...
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| Veröffentlicht in: | The Astrophysical journal 2021-09, Vol.919 (1), p.45 |
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| creator | Bergner, Jennifer B. Ciesla, Fred |
| description | The compositions of planet-forming disks are set by a combination of material inherited from the interstellar medium and material reprocessed during disk formation and evolution. Indeed, comets and primitive meteorites exhibit interstellar-like isotopic ratios and/or volatile compositions, supporting that some pristine material was incorporated intact into icy planetesimals in the solar nebula. To date, the survival of volatile interstellar material in the disk stage has not been modeled using realistic disk physics. Here, we present a modeling framework to track the destruction of interstellar ices on dust grains undergoing transport processes within a disk, with a particular focus on explaining the incorporation of pristine material into icy planetesimals. We find that it is difficult to explain inheritance through the local assembly of comets, as ice destruction is rapid for small ( |
| doi_str_mv | 10.3847/1538-4357/ac0fd7 |
| format | Article |
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μ
m) grains in the inner few tens of au. Instead, a plausible pathway to inheritance is to form pebbles at larger disk radii, which then drift inward to the comet-forming zone with their ices mostly preserved. Small grains beyond ∼100 au can experience ice photodissociation at the tens of percent level; however, little of the ice is actually lost from the grain, likely making this a robust site for in situ ice chemistry. Our models also indicate that many complex organic species should survive passage through the disk intact. This raises the possibility that organics synthesized in the interstellar medium can be delivered to terrestrial planets by icy-body impact and thus potentially participate in origins of life chemistry.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ac0fd7</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion disks ; Astrochemistry ; Astrophysics ; Comet origins ; Comets ; Destruction ; Grains ; Ice ; Inheritances ; Interstellar ices ; Interstellar matter ; Interstellar medium ; Isotope ratios ; Modelling ; Photodissociation ; Planet formation ; Planetary composition ; Protoplanetary disks ; Solar nebula ; Terrestrial environments ; Terrestrial planets ; Transport processes</subject><ispartof>The Astrophysical journal, 2021-09, Vol.919 (1), p.45</ispartof><rights>2021. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Sep 01, 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c379t-a7ee61b68e00f3514aaba5173e59d2d1970215f45792e89af618b6da33c82aec3</citedby><cites>FETCH-LOGICAL-c379t-a7ee61b68e00f3514aaba5173e59d2d1970215f45792e89af618b6da33c82aec3</cites><orcidid>0000-0002-8716-0482 ; 0000-0002-0093-065X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ac0fd7/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ac0fd7$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Bergner, Jennifer B.</creatorcontrib><creatorcontrib>Ciesla, Fred</creatorcontrib><title>Ice Inheritance in Dynamical Disk Models</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The compositions of planet-forming disks are set by a combination of material inherited from the interstellar medium and material reprocessed during disk formation and evolution. Indeed, comets and primitive meteorites exhibit interstellar-like isotopic ratios and/or volatile compositions, supporting that some pristine material was incorporated intact into icy planetesimals in the solar nebula. To date, the survival of volatile interstellar material in the disk stage has not been modeled using realistic disk physics. Here, we present a modeling framework to track the destruction of interstellar ices on dust grains undergoing transport processes within a disk, with a particular focus on explaining the incorporation of pristine material into icy planetesimals. We find that it is difficult to explain inheritance through the local assembly of comets, as ice destruction is rapid for small (<10
μ
m) grains in the inner few tens of au. Instead, a plausible pathway to inheritance is to form pebbles at larger disk radii, which then drift inward to the comet-forming zone with their ices mostly preserved. Small grains beyond ∼100 au can experience ice photodissociation at the tens of percent level; however, little of the ice is actually lost from the grain, likely making this a robust site for in situ ice chemistry. Our models also indicate that many complex organic species should survive passage through the disk intact. This raises the possibility that organics synthesized in the interstellar medium can be delivered to terrestrial planets by icy-body impact and thus potentially participate in origins of life chemistry.</description><subject>Accretion disks</subject><subject>Astrochemistry</subject><subject>Astrophysics</subject><subject>Comet origins</subject><subject>Comets</subject><subject>Destruction</subject><subject>Grains</subject><subject>Ice</subject><subject>Inheritances</subject><subject>Interstellar ices</subject><subject>Interstellar matter</subject><subject>Interstellar medium</subject><subject>Isotope ratios</subject><subject>Modelling</subject><subject>Photodissociation</subject><subject>Planet formation</subject><subject>Planetary composition</subject><subject>Protoplanetary disks</subject><subject>Solar nebula</subject><subject>Terrestrial environments</subject><subject>Terrestrial planets</subject><subject>Transport processes</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp9kEtLxDAUhYMoWEf3Lgu6cGGdpEmaZCkzPgojbhTchds0wdZOW5POYv69LRXdiKv74Dv3cg5C5wTfUMnEknAqE0a5WILBrhQHKPpZHaIIY8ySjIq3Y3QSQj2NqVIRusqNjfP23fpqgHbsqzZe71vYVgaaeF2Fj_ipK20TTtGRgybYs--6QK_3dy-rx2Tz_JCvbjeJoUINCQhrM1Jk0mLsKCcMoABOBLVclWlJlMAp4Y5xoVIrFbiMyCIrgVIjU7CGLtDFfLf33efOhkHX3c6340udciFwxoikI4VnyvguBG-d7n21Bb_XBOspDz2Z15N5PecxSq5nSdX1vzf_wS__wKGvtSJKE8247ktHvwDSwmwe</recordid><startdate>20210901</startdate><enddate>20210901</enddate><creator>Bergner, Jennifer B.</creator><creator>Ciesla, Fred</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-8716-0482</orcidid><orcidid>https://orcid.org/0000-0002-0093-065X</orcidid></search><sort><creationdate>20210901</creationdate><title>Ice Inheritance in Dynamical Disk Models</title><author>Bergner, Jennifer B. ; Ciesla, Fred</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c379t-a7ee61b68e00f3514aaba5173e59d2d1970215f45792e89af618b6da33c82aec3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Accretion disks</topic><topic>Astrochemistry</topic><topic>Astrophysics</topic><topic>Comet origins</topic><topic>Comets</topic><topic>Destruction</topic><topic>Grains</topic><topic>Ice</topic><topic>Inheritances</topic><topic>Interstellar ices</topic><topic>Interstellar matter</topic><topic>Interstellar medium</topic><topic>Isotope ratios</topic><topic>Modelling</topic><topic>Photodissociation</topic><topic>Planet formation</topic><topic>Planetary composition</topic><topic>Protoplanetary disks</topic><topic>Solar nebula</topic><topic>Terrestrial environments</topic><topic>Terrestrial planets</topic><topic>Transport processes</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bergner, Jennifer B.</creatorcontrib><creatorcontrib>Ciesla, Fred</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Bergner, Jennifer B.</au><au>Ciesla, Fred</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Ice Inheritance in Dynamical Disk Models</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2021-09-01</date><risdate>2021</risdate><volume>919</volume><issue>1</issue><spage>45</spage><pages>45-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The compositions of planet-forming disks are set by a combination of material inherited from the interstellar medium and material reprocessed during disk formation and evolution. Indeed, comets and primitive meteorites exhibit interstellar-like isotopic ratios and/or volatile compositions, supporting that some pristine material was incorporated intact into icy planetesimals in the solar nebula. To date, the survival of volatile interstellar material in the disk stage has not been modeled using realistic disk physics. Here, we present a modeling framework to track the destruction of interstellar ices on dust grains undergoing transport processes within a disk, with a particular focus on explaining the incorporation of pristine material into icy planetesimals. We find that it is difficult to explain inheritance through the local assembly of comets, as ice destruction is rapid for small (<10
μ
m) grains in the inner few tens of au. Instead, a plausible pathway to inheritance is to form pebbles at larger disk radii, which then drift inward to the comet-forming zone with their ices mostly preserved. Small grains beyond ∼100 au can experience ice photodissociation at the tens of percent level; however, little of the ice is actually lost from the grain, likely making this a robust site for in situ ice chemistry. Our models also indicate that many complex organic species should survive passage through the disk intact. This raises the possibility that organics synthesized in the interstellar medium can be delivered to terrestrial planets by icy-body impact and thus potentially participate in origins of life chemistry.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ac0fd7</doi><tpages>16</tpages><orcidid>https://orcid.org/0000-0002-8716-0482</orcidid><orcidid>https://orcid.org/0000-0002-0093-065X</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Accretion disks Astrochemistry Astrophysics Comet origins Comets Destruction Grains Ice Inheritances Interstellar ices Interstellar matter Interstellar medium Isotope ratios Modelling Photodissociation Planet formation Planetary composition Protoplanetary disks Solar nebula Terrestrial environments Terrestrial planets Transport processes |
| title | Ice Inheritance in Dynamical Disk Models |
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