Meridional flows in the disk around a young star
Protoplanetary disks are known to possess a variety of substructures in the distribution of their millimetre-sized grains, predominantly seen as rings and gaps 1 , which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk...
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| Veröffentlicht in: | Nature (London) 2019-10, Vol.574 (7778), p.378-381 |
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| creator | Teague, Richard Bae, Jaehan Bergin, Edwin A. |
| description | Protoplanetary disks are known to possess a variety of substructures in the distribution of their millimetre-sized grains, predominantly seen as rings and gaps
1
, which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk
2
or (magneto-)hydrodynamic instabilities
3
. The velocity structure of the gas offers a unique probe of both the underlying mechanisms driving the evolution of the disk—such as movement of planet-building material from volatile-rich regions to the chemically inert midplane—and the details of the required removal of angular momentum. Here we report radial profiles of the three velocity components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission from
12
CO molecules. These velocities reveal substantial flows from the surface of the disk towards its midplane at the radial locations of gaps that have been argued to be opened by embedded planets
4
–
7
: these flows bear a striking resemblance to meridional flows, long predicted to occur during the early stages of planet formation
8
–
12
. In addition, a persistent radial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated with previously detected extended emission
12
.
Three-dimensional gas velocities in the gapped disk around the young star HD 163296 show meridional flows from the surface of the disk towards its midplane at gap locations. |
| doi_str_mv | 10.1038/s41586-019-1642-0 |
| format | Article |
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1
, which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk
2
or (magneto-)hydrodynamic instabilities
3
. The velocity structure of the gas offers a unique probe of both the underlying mechanisms driving the evolution of the disk—such as movement of planet-building material from volatile-rich regions to the chemically inert midplane—and the details of the required removal of angular momentum. Here we report radial profiles of the three velocity components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission from
12
CO molecules. These velocities reveal substantial flows from the surface of the disk towards its midplane at the radial locations of gaps that have been argued to be opened by embedded planets
4
–
7
: these flows bear a striking resemblance to meridional flows, long predicted to occur during the early stages of planet formation
8
–
12
. In addition, a persistent radial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated with previously detected extended emission
12
.
Three-dimensional gas velocities in the gapped disk around the young star HD 163296 show meridional flows from the surface of the disk towards its midplane at gap locations.</description><identifier>ISSN: 0028-0836</identifier><identifier>EISSN: 1476-4687</identifier><identifier>DOI: 10.1038/s41586-019-1642-0</identifier><identifier>PMID: 31619790</identifier><language>eng</language><publisher>London: Nature Publishing Group UK</publisher><subject>639/33/34/4122 ; 639/33/34/862 ; Accretion disks ; Angular momentum ; Angular velocity ; Construction materials ; Humanities and Social Sciences ; Letter ; Meridional flow ; multidisciplinary ; Natural history ; Organic chemistry ; Outflow ; Planet formation ; Planets ; Protoplanetary disks ; Protoplanets ; Science ; Science (multidisciplinary) ; Stars ; Stellar winds ; Substructures ; Velocity</subject><ispartof>Nature (London), 2019-10, Vol.574 (7778), p.378-381</ispartof><rights>The Author(s), under exclusive licence to Springer Nature Limited 2019</rights><rights>COPYRIGHT 2019 Nature Publishing Group</rights><rights>Copyright Nature Publishing Group Oct 17, 2019</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c640t-769e3c2a1a5afbac041ccc73a938b5d92e85a50e86d555754daa1a5b354a63b03</citedby><cites>FETCH-LOGICAL-c640t-769e3c2a1a5afbac041ccc73a938b5d92e85a50e86d555754daa1a5b354a63b03</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1038/s41586-019-1642-0$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1038/s41586-019-1642-0$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/31619790$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink></links><search><creatorcontrib>Teague, Richard</creatorcontrib><creatorcontrib>Bae, Jaehan</creatorcontrib><creatorcontrib>Bergin, Edwin A.</creatorcontrib><title>Meridional flows in the disk around a young star</title><title>Nature (London)</title><addtitle>Nature</addtitle><addtitle>Nature</addtitle><description>Protoplanetary disks are known to possess a variety of substructures in the distribution of their millimetre-sized grains, predominantly seen as rings and gaps
1
, which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk
2
or (magneto-)hydrodynamic instabilities
3
. The velocity structure of the gas offers a unique probe of both the underlying mechanisms driving the evolution of the disk—such as movement of planet-building material from volatile-rich regions to the chemically inert midplane—and the details of the required removal of angular momentum. Here we report radial profiles of the three velocity components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission from
12
CO molecules. These velocities reveal substantial flows from the surface of the disk towards its midplane at the radial locations of gaps that have been argued to be opened by embedded planets
4
–
7
: these flows bear a striking resemblance to meridional flows, long predicted to occur during the early stages of planet formation
8
–
12
. In addition, a persistent radial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated with previously detected extended emission
12
.
Three-dimensional gas velocities in the gapped disk around the young star HD 163296 show meridional flows from the surface of the disk towards its midplane at gap locations.</description><subject>639/33/34/4122</subject><subject>639/33/34/862</subject><subject>Accretion disks</subject><subject>Angular momentum</subject><subject>Angular velocity</subject><subject>Construction materials</subject><subject>Humanities and Social Sciences</subject><subject>Letter</subject><subject>Meridional flow</subject><subject>multidisciplinary</subject><subject>Natural history</subject><subject>Organic chemistry</subject><subject>Outflow</subject><subject>Planet formation</subject><subject>Planets</subject><subject>Protoplanetary disks</subject><subject>Protoplanets</subject><subject>Science</subject><subject>Science (multidisciplinary)</subject><subject>Stars</subject><subject>Stellar 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(London)</jtitle><stitle>Nature</stitle><addtitle>Nature</addtitle><date>2019-10</date><risdate>2019</risdate><volume>574</volume><issue>7778</issue><spage>378</spage><epage>381</epage><pages>378-381</pages><issn>0028-0836</issn><eissn>1476-4687</eissn><abstract>Protoplanetary disks are known to possess a variety of substructures in the distribution of their millimetre-sized grains, predominantly seen as rings and gaps
1
, which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk
2
or (magneto-)hydrodynamic instabilities
3
. The velocity structure of the gas offers a unique probe of both the underlying mechanisms driving the evolution of the disk—such as movement of planet-building material from volatile-rich regions to the chemically inert midplane—and the details of the required removal of angular momentum. Here we report radial profiles of the three velocity components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission from
12
CO molecules. These velocities reveal substantial flows from the surface of the disk towards its midplane at the radial locations of gaps that have been argued to be opened by embedded planets
4
–
7
: these flows bear a striking resemblance to meridional flows, long predicted to occur during the early stages of planet formation
8
–
12
. In addition, a persistent radial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated with previously detected extended emission
12
.
Three-dimensional gas velocities in the gapped disk around the young star HD 163296 show meridional flows from the surface of the disk towards its midplane at gap locations.</abstract><cop>London</cop><pub>Nature Publishing Group UK</pub><pmid>31619790</pmid><doi>10.1038/s41586-019-1642-0</doi><tpages>4</tpages></addata></record> |
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| ispartof | Nature (London), 2019-10, Vol.574 (7778), p.378-381 |
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| source | SpringerLink Journals; Nature Journals Online |
| subjects | 639/33/34/4122 639/33/34/862 Accretion disks Angular momentum Angular velocity Construction materials Humanities and Social Sciences Letter Meridional flow multidisciplinary Natural history Organic chemistry Outflow Planet formation Planets Protoplanetary disks Protoplanets Science Science (multidisciplinary) Stars Stellar winds Substructures Velocity |
| title | Meridional flows in the disk around a young star |
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