Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?
A leading theoretical expectation for the final stages of planet formation is that disk migration should naturally drive orbits into chains of mean motion resonances (MMRs). In order to explain the dearth of MMR chains observed at Gyr ages (
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| Veröffentlicht in: | Astrophysical journal. Letters 2022-06, Vol.932 (1), p.L12 |
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| creator | Tejada Arevalo, Roberto Tamayo, Daniel Cranmer, Miles |
| description | A leading theoretical expectation for the final stages of planet formation is that disk migration should naturally drive orbits into chains of mean motion resonances (MMRs). In order to explain the dearth of MMR chains observed at Gyr ages ( |
| doi_str_mv | 10.3847/2041-8213/ac70e0 |
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b
places it within a factor of 2 of the instability limit, and that this allows us to set significantly lower limits on the eccentricity (
e
b
≤0.17 at 99.7% confidence). Additionally, we rule out a resonant chain configuration for V1298 Tau at ≳99% confidence. Thus, if the ∼23 Myr old V1298 Tau system did form as a resonant chain, it must have undergone instability and rearrangement shortly after disk dispersal. We expect that similar stability constrained characterization of future young multiplanet systems will be valuable in informing planet formation models.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/ac70e0</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Chain drives ; Configurations ; Constraints ; Dispersal ; Dispersion ; Dynamic stability ; Exoplanet dynamics ; Exoplanet evolution ; Exoplanet formation ; Orbital resonances ; Orbital resonances (celestial mechanics) ; Orbits ; Planet formation ; Planets ; Radial velocity</subject><ispartof>Astrophysical journal. Letters, 2022-06, Vol.932 (1), p.L12</ispartof><rights>2022. The Author(s). Published by the American Astronomical Society.</rights><rights>2022. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c381t-bf49523551c048f3f2f3490368932aa4e1ea127ba221cb4bebb417f716e84ce73</citedby><cites>FETCH-LOGICAL-c381t-bf49523551c048f3f2f3490368932aa4e1ea127ba221cb4bebb417f716e84ce73</cites><orcidid>0000-0002-9908-8705 ; 0000-0002-6458-3423 ; 0000-0001-6708-3427</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/ac70e0/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,27901,27902,38845,38867,53815,53842</link.rule.ids></links><search><creatorcontrib>Tejada Arevalo, Roberto</creatorcontrib><creatorcontrib>Tamayo, Daniel</creatorcontrib><creatorcontrib>Cranmer, Miles</creatorcontrib><title>Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>A leading theoretical expectation for the final stages of planet formation is that disk migration should naturally drive orbits into chains of mean motion resonances (MMRs). In order to explain the dearth of MMR chains observed at Gyr ages (<1%), this picture requires such configurations to destabilize and scramble period ratios following disk dispersal. Strikingly, the only two known stars with three or more planets younger than ≲100 Myr, HR 8799 and V1298 Tau, have been suggested to be in such MMR chains, given the orbits’ near-integer period ratios. We incorporate recent transit and radial velocity (RV) observations of the V1298 Tau system, and investigate constraints on the system’s orbital architecture imposed by requiring dynamical stability on timescales much shorter than the system’s age. We show that the recent RV mass measurement of V1298 Tau
b
places it within a factor of 2 of the instability limit, and that this allows us to set significantly lower limits on the eccentricity (
e
b
≤0.17 at 99.7% confidence). Additionally, we rule out a resonant chain configuration for V1298 Tau at ≳99% confidence. Thus, if the ∼23 Myr old V1298 Tau system did form as a resonant chain, it must have undergone instability and rearrangement shortly after disk dispersal. We expect that similar stability constrained characterization of future young multiplanet systems will be valuable in informing planet formation models.</description><subject>Chain drives</subject><subject>Configurations</subject><subject>Constraints</subject><subject>Dispersal</subject><subject>Dispersion</subject><subject>Dynamic stability</subject><subject>Exoplanet dynamics</subject><subject>Exoplanet evolution</subject><subject>Exoplanet formation</subject><subject>Orbital resonances</subject><subject>Orbital resonances (celestial mechanics)</subject><subject>Orbits</subject><subject>Planet formation</subject><subject>Planets</subject><subject>Radial velocity</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><recordid>eNp9kMtLAzEQxhdRUKt3jwHBk9W8djf1IlKfUFF8gacwu51oyjZZk_RQb_7nbq3oRbzMDMNvvo_5smyH0QOhZHnIqWR9xZk4hLqkSFeyjZ_V6s9M8_VsM8YJpZwWTG1kH_cJKtvYNCdD72IKYB2OyfAVAtQJg32HZL0j3pD0ioQLcj0P5KYZkyfGB4o8wIzcz2PC6RE59eTZz9wLuW3AYYrk3IcpsY5cI3TFfwndYfQOXI0LD-vi8Va2ZqCJuP3de9nj-dnD8LI_urm4Gp6M-rVQLPUrIwc5F3nOaiqVEYYbIQdUFGogOIBEhsB4WQHnrK5khVUlWWlKVqCSNZail-0uddvg32YYk574WXCdpeZFqajKVSE7ii6pOvgYAxrdBjuFMNeM6kXQepGkXqSql0F3J_vLE-vbX81_8L0_cGgnje4-0UyPGNft2IhPhSmKpA</recordid><startdate>20220601</startdate><enddate>20220601</enddate><creator>Tejada Arevalo, Roberto</creator><creator>Tamayo, Daniel</creator><creator>Cranmer, Miles</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><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/0000-0002-9908-8705</orcidid><orcidid>https://orcid.org/0000-0002-6458-3423</orcidid><orcidid>https://orcid.org/0000-0001-6708-3427</orcidid></search><sort><creationdate>20220601</creationdate><title>Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?</title><author>Tejada Arevalo, Roberto ; Tamayo, Daniel ; Cranmer, Miles</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c381t-bf49523551c048f3f2f3490368932aa4e1ea127ba221cb4bebb417f716e84ce73</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Chain drives</topic><topic>Configurations</topic><topic>Constraints</topic><topic>Dispersal</topic><topic>Dispersion</topic><topic>Dynamic stability</topic><topic>Exoplanet dynamics</topic><topic>Exoplanet evolution</topic><topic>Exoplanet formation</topic><topic>Orbital resonances</topic><topic>Orbital resonances (celestial mechanics)</topic><topic>Orbits</topic><topic>Planet formation</topic><topic>Planets</topic><topic>Radial velocity</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Tejada Arevalo, Roberto</creatorcontrib><creatorcontrib>Tamayo, Daniel</creatorcontrib><creatorcontrib>Cranmer, Miles</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><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>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Tejada Arevalo, Roberto</au><au>Tamayo, Daniel</au><au>Cranmer, Miles</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2022-06-01</date><risdate>2022</risdate><volume>932</volume><issue>1</issue><spage>L12</spage><pages>L12-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>A leading theoretical expectation for the final stages of planet formation is that disk migration should naturally drive orbits into chains of mean motion resonances (MMRs). In order to explain the dearth of MMR chains observed at Gyr ages (<1%), this picture requires such configurations to destabilize and scramble period ratios following disk dispersal. Strikingly, the only two known stars with three or more planets younger than ≲100 Myr, HR 8799 and V1298 Tau, have been suggested to be in such MMR chains, given the orbits’ near-integer period ratios. We incorporate recent transit and radial velocity (RV) observations of the V1298 Tau system, and investigate constraints on the system’s orbital architecture imposed by requiring dynamical stability on timescales much shorter than the system’s age. We show that the recent RV mass measurement of V1298 Tau
b
places it within a factor of 2 of the instability limit, and that this allows us to set significantly lower limits on the eccentricity (
e
b
≤0.17 at 99.7% confidence). Additionally, we rule out a resonant chain configuration for V1298 Tau at ≳99% confidence. Thus, if the ∼23 Myr old V1298 Tau system did form as a resonant chain, it must have undergone instability and rearrangement shortly after disk dispersal. We expect that similar stability constrained characterization of future young multiplanet systems will be valuable in informing planet formation models.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/ac70e0</doi><tpages>8</tpages><orcidid>https://orcid.org/0000-0002-9908-8705</orcidid><orcidid>https://orcid.org/0000-0002-6458-3423</orcidid><orcidid>https://orcid.org/0000-0001-6708-3427</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Chain drives Configurations Constraints Dispersal Dispersion Dynamic stability Exoplanet dynamics Exoplanet evolution Exoplanet formation Orbital resonances Orbital resonances (celestial mechanics) Orbits Planet formation Planets Radial velocity |
| title | Stability Constrained Characterization of the 23 Myr Old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains? |
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