Magnetospheric Accretion as a Source of Hα Emission from Protoplanets around PDS 70
Advances in high-resolution imaging have revealed H α emission separate from the host star. It is generally believed that the emission is associated with planets forming in protoplanetary disks. However, the nature of this emission is still not fully understood. Here we report a modeling of H α emis...
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| Veröffentlicht in: | The Astrophysical journal 2019-11, Vol.885 (1), p.94 |
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| creator | Thanathibodee, Thanawuth Calvet, Nuria Bae, Jaehan Muzerolle, James Hernández, Ramiro Franco |
| description | Advances in high-resolution imaging have revealed H
α
emission separate from the host star. It is generally believed that the emission is associated with planets forming in protoplanetary disks. However, the nature of this emission is still not fully understood. Here we report a modeling of H
α
emission from the planets around the young star PDS 70. Using standard magnetospheric accretion models previously applied to accreting young stars, we find that the observed line fluxes can be reproduced using a range of parameters relevant to PDS 70b and c, with a mean mass accretion rate of log(
) = −8.0 ± 0.6
M
Jup
yr
−1
and −8.1 ± 0.6
M
Jup
yr
−1
for PDS 70b and PDS 70c, respectively. Our results suggest that H
α
emission from young planets can originate in the magnetospheric accretion of mass from the circumplanetary disk. We find that empirical relationships between mass accretion rate and H
α
line properties frequently used in T Tauri stars are not applicable in the planetary mass regime. In particular, the correlations between line flux and mass accretion rate underpredict the accretion rate by about an order of magnitude, and the width at the 10% height of the line is insensitive to the accretion rate at
|
| doi_str_mv | 10.3847/1538-4357/ab44c1 |
| format | Article |
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α
emission separate from the host star. It is generally believed that the emission is associated with planets forming in protoplanetary disks. However, the nature of this emission is still not fully understood. Here we report a modeling of H
α
emission from the planets around the young star PDS 70. Using standard magnetospheric accretion models previously applied to accreting young stars, we find that the observed line fluxes can be reproduced using a range of parameters relevant to PDS 70b and c, with a mean mass accretion rate of log(
) = −8.0 ± 0.6
M
Jup
yr
−1
and −8.1 ± 0.6
M
Jup
yr
−1
for PDS 70b and PDS 70c, respectively. Our results suggest that H
α
emission from young planets can originate in the magnetospheric accretion of mass from the circumplanetary disk. We find that empirical relationships between mass accretion rate and H
α
line properties frequently used in T Tauri stars are not applicable in the planetary mass regime. In particular, the correlations between line flux and mass accretion rate underpredict the accretion rate by about an order of magnitude, and the width at the 10% height of the line is insensitive to the accretion rate at
< 10
−8
M
Jup
yr
−1
.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab44c1</identifier><language>eng</language><publisher>Philadelphia: IOP Publishing</publisher><subject>Accretion disks ; Astrophysics ; Deposition ; Emission ; Fluxes ; H alpha line ; Image resolution ; Magnetospheres ; Planet formation ; Planetary mass ; Planets ; Protoplanetary disks ; Protoplanets ; Stars ; T Tauri stars</subject><ispartof>The Astrophysical journal, 2019-11, Vol.885 (1), p.94</ispartof><rights>Copyright IOP Publishing Nov 01, 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c2281-924183d1ef504d8c359a7dc7e8e8fa3e4222264ae4b0fb79d2f55160087260283</citedby><cites>FETCH-LOGICAL-c2281-924183d1ef504d8c359a7dc7e8e8fa3e4222264ae4b0fb79d2f55160087260283</cites><orcidid>0000-0003-4507-1710 ; 0000-0002-3950-5386 ; 0000-0001-7258-770X ; 0000-0002-1650-3740 ; 0000-0002-5943-1222</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids></links><search><creatorcontrib>Thanathibodee, Thanawuth</creatorcontrib><creatorcontrib>Calvet, Nuria</creatorcontrib><creatorcontrib>Bae, Jaehan</creatorcontrib><creatorcontrib>Muzerolle, James</creatorcontrib><creatorcontrib>Hernández, Ramiro Franco</creatorcontrib><title>Magnetospheric Accretion as a Source of Hα Emission from Protoplanets around PDS 70</title><title>The Astrophysical journal</title><description>Advances in high-resolution imaging have revealed H
α
emission separate from the host star. It is generally believed that the emission is associated with planets forming in protoplanetary disks. However, the nature of this emission is still not fully understood. Here we report a modeling of H
α
emission from the planets around the young star PDS 70. Using standard magnetospheric accretion models previously applied to accreting young stars, we find that the observed line fluxes can be reproduced using a range of parameters relevant to PDS 70b and c, with a mean mass accretion rate of log(
) = −8.0 ± 0.6
M
Jup
yr
−1
and −8.1 ± 0.6
M
Jup
yr
−1
for PDS 70b and PDS 70c, respectively. Our results suggest that H
α
emission from young planets can originate in the magnetospheric accretion of mass from the circumplanetary disk. We find that empirical relationships between mass accretion rate and H
α
line properties frequently used in T Tauri stars are not applicable in the planetary mass regime. In particular, the correlations between line flux and mass accretion rate underpredict the accretion rate by about an order of magnitude, and the width at the 10% height of the line is insensitive to the accretion rate at
< 10
−8
M
Jup
yr
−1
.</description><subject>Accretion disks</subject><subject>Astrophysics</subject><subject>Deposition</subject><subject>Emission</subject><subject>Fluxes</subject><subject>H alpha line</subject><subject>Image resolution</subject><subject>Magnetospheres</subject><subject>Planet formation</subject><subject>Planetary mass</subject><subject>Planets</subject><subject>Protoplanetary disks</subject><subject>Protoplanets</subject><subject>Stars</subject><subject>T Tauri stars</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNo9kM9OwzAMxiMEEmVw5xiJc1n-NulxGmNDGmLShsQtStMEOq1NSboDj8WL8EykGsIXy_bnz9YPgFuM7qlkYoo5lTmjXEx1xZjBZyD7b52DDCHE8oKKt0twFeN-LElZZmD3rN87O_jYf9jQGDgzJtih8R3UEWq49cdgLPQOrn6-4aJtYhxnLvgWboIffH_QaT1Jgz92Ndw8bKFA1-DC6UO0N395Al4fF7v5Kl-_LJ_ms3VuCJE4LwnDktbYOo5YLQ3lpRa1EVZa6TS1jKQomLasQq4SZU0c57hASApSICLpBNydfPvgP482Dmqf_u3SSUVowRMWiWlSoZPKBB9jsE71oWl1-FIYqZGdGkGpEZQ6saO_LzhhAg</recordid><startdate>20191101</startdate><enddate>20191101</enddate><creator>Thanathibodee, Thanawuth</creator><creator>Calvet, Nuria</creator><creator>Bae, Jaehan</creator><creator>Muzerolle, James</creator><creator>Hernández, Ramiro Franco</creator><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/0000-0003-4507-1710</orcidid><orcidid>https://orcid.org/0000-0002-3950-5386</orcidid><orcidid>https://orcid.org/0000-0001-7258-770X</orcidid><orcidid>https://orcid.org/0000-0002-1650-3740</orcidid><orcidid>https://orcid.org/0000-0002-5943-1222</orcidid></search><sort><creationdate>20191101</creationdate><title>Magnetospheric Accretion as a Source of Hα Emission from Protoplanets around PDS 70</title><author>Thanathibodee, Thanawuth ; Calvet, Nuria ; Bae, Jaehan ; Muzerolle, James ; Hernández, Ramiro Franco</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c2281-924183d1ef504d8c359a7dc7e8e8fa3e4222264ae4b0fb79d2f55160087260283</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Accretion disks</topic><topic>Astrophysics</topic><topic>Deposition</topic><topic>Emission</topic><topic>Fluxes</topic><topic>H alpha line</topic><topic>Image resolution</topic><topic>Magnetospheres</topic><topic>Planet formation</topic><topic>Planetary mass</topic><topic>Planets</topic><topic>Protoplanetary disks</topic><topic>Protoplanets</topic><topic>Stars</topic><topic>T Tauri stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Thanathibodee, Thanawuth</creatorcontrib><creatorcontrib>Calvet, Nuria</creatorcontrib><creatorcontrib>Bae, Jaehan</creatorcontrib><creatorcontrib>Muzerolle, James</creatorcontrib><creatorcontrib>Hernández, Ramiro Franco</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</fulltext></delivery><addata><au>Thanathibodee, Thanawuth</au><au>Calvet, Nuria</au><au>Bae, Jaehan</au><au>Muzerolle, James</au><au>Hernández, Ramiro Franco</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Magnetospheric Accretion as a Source of Hα Emission from Protoplanets around PDS 70</atitle><jtitle>The Astrophysical journal</jtitle><date>2019-11-01</date><risdate>2019</risdate><volume>885</volume><issue>1</issue><spage>94</spage><pages>94-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Advances in high-resolution imaging have revealed H
α
emission separate from the host star. It is generally believed that the emission is associated with planets forming in protoplanetary disks. However, the nature of this emission is still not fully understood. Here we report a modeling of H
α
emission from the planets around the young star PDS 70. Using standard magnetospheric accretion models previously applied to accreting young stars, we find that the observed line fluxes can be reproduced using a range of parameters relevant to PDS 70b and c, with a mean mass accretion rate of log(
) = −8.0 ± 0.6
M
Jup
yr
−1
and −8.1 ± 0.6
M
Jup
yr
−1
for PDS 70b and PDS 70c, respectively. Our results suggest that H
α
emission from young planets can originate in the magnetospheric accretion of mass from the circumplanetary disk. We find that empirical relationships between mass accretion rate and H
α
line properties frequently used in T Tauri stars are not applicable in the planetary mass regime. In particular, the correlations between line flux and mass accretion rate underpredict the accretion rate by about an order of magnitude, and the width at the 10% height of the line is insensitive to the accretion rate at
< 10
−8
M
Jup
yr
−1
.</abstract><cop>Philadelphia</cop><pub>IOP Publishing</pub><doi>10.3847/1538-4357/ab44c1</doi><orcidid>https://orcid.org/0000-0003-4507-1710</orcidid><orcidid>https://orcid.org/0000-0002-3950-5386</orcidid><orcidid>https://orcid.org/0000-0001-7258-770X</orcidid><orcidid>https://orcid.org/0000-0002-1650-3740</orcidid><orcidid>https://orcid.org/0000-0002-5943-1222</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | The Astrophysical journal, 2019-11, Vol.885 (1), p.94 |
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| language | eng |
| recordid | cdi_proquest_journals_2365847813 |
| source | IOP Publishing Free Content; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Accretion disks Astrophysics Deposition Emission Fluxes H alpha line Image resolution Magnetospheres Planet formation Planetary mass Planets Protoplanetary disks Protoplanets Stars T Tauri stars |
| title | Magnetospheric Accretion as a Source of Hα Emission from Protoplanets around PDS 70 |
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