Interferometric Identification of a Pre-Brown Dwarf
It is not known whether brown dwarfs [stellar-like objects with masses less than the hydrogen-burning limit, 0.075 solar mass (M[Symbol])] are formed in the same way as solar-type stars or by some other process. Here we report the clear-cut identification of a self-gravitating condensation of gas an...
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| Veröffentlicht in: | Science (American Association for the Advancement of Science) 2012-07, Vol.337 (6090), p.69-72 |
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| container_issue | 6090 |
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| container_title | Science (American Association for the Advancement of Science) |
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| creator | André, Philippe Ward-Thompson, Derek Greaves, Jane |
| description | It is not known whether brown dwarfs [stellar-like objects with masses less than the hydrogen-burning limit, 0.075 solar mass (M[Symbol])] are formed in the same way as solar-type stars or by some other process. Here we report the clear-cut identification of a self-gravitating condensation of gas and dust with a mass in the brown-dwarf regime, made through millimeter interferometric observations. The level of thermal millimeter continuum emission detected from this object indicates a mass -0.02 to 0.03 M[Symbol], whereas the small radius, < 460 astronomical units, and narrow spectral lines imply a dynamical mass of 0.015 to 0.02 M[Symbol]. The identification of such a pre-brown dwarf core supports models according to which brown dwarfs are formed in the same manner as hydrogen-burning stars. |
| doi_str_mv | 10.1126/science.1222602 |
| format | Article |
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Here we report the clear-cut identification of a self-gravitating condensation of gas and dust with a mass in the brown-dwarf regime, made through millimeter interferometric observations. The level of thermal millimeter continuum emission detected from this object indicates a mass -0.02 to 0.03 M[Symbol], whereas the small radius, < 460 astronomical units, and narrow spectral lines imply a dynamical mass of 0.015 to 0.02 M[Symbol]. The identification of such a pre-brown dwarf core supports models according to which brown dwarfs are formed in the same manner as hydrogen-burning stars.</description><identifier>ISSN: 0036-8075</identifier><identifier>EISSN: 1095-9203</identifier><identifier>DOI: 10.1126/science.1222602</identifier><identifier>PMID: 22767923</identifier><identifier>CODEN: SCIEAS</identifier><language>eng</language><publisher>Washington, DC: American Association for the Advancement of Science</publisher><subject>Alps ; Astronomical objects ; Astronomical observations ; Astronomy ; Average linear density ; Brown dwarf stars ; Brown dwarfs ; Dwarf stars ; Earth, ocean, space ; Exact sciences and technology ; Extrasolar planets ; Fine structure ; Flux density ; Forming ; Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations ; Geometric lines ; Interferometers ; Interferometry ; Low luminosity stars, subdwarfs, and brown dwarfs ; Mass ; Normal stars (by class): general or individual ; Protostars ; Radio, microwave (> 1 mm) ; Stars ; Stellar masses ; Sun</subject><ispartof>Science (American Association for the Advancement of Science), 2012-07, Vol.337 (6090), p.69-72</ispartof><rights>Copyright © 2012 American Association for the Advancement of Science</rights><rights>2015 INIST-CNRS</rights><rights>Copyright © 2012, American Association for the Advancement of Science</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c476t-95f8a536ef18b9c4e57d0192f96d14c99cc1a02d504f3eb3bcb4d6db648009263</citedby><cites>FETCH-LOGICAL-c476t-95f8a536ef18b9c4e57d0192f96d14c99cc1a02d504f3eb3bcb4d6db648009263</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://www.jstor.org/stable/pdf/41585205$$EPDF$$P50$$Gjstor$$H</linktopdf><linktohtml>$$Uhttps://www.jstor.org/stable/41585205$$EHTML$$P50$$Gjstor$$H</linktohtml><link.rule.ids>314,776,780,799,2871,2872,27901,27902,57992,58225</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=26103641$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/22767923$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink></links><search><creatorcontrib>André, Philippe</creatorcontrib><creatorcontrib>Ward-Thompson, Derek</creatorcontrib><creatorcontrib>Greaves, Jane</creatorcontrib><title>Interferometric Identification of a Pre-Brown Dwarf</title><title>Science (American Association for the Advancement of Science)</title><addtitle>Science</addtitle><description>It is not known whether brown dwarfs [stellar-like objects with masses less than the hydrogen-burning limit, 0.075 solar mass (M[Symbol])] are formed in the same way as solar-type stars or by some other process. 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The identification of such a pre-brown dwarf core supports models according to which brown dwarfs are formed in the same manner as hydrogen-burning stars.</description><subject>Alps</subject><subject>Astronomical objects</subject><subject>Astronomical observations</subject><subject>Astronomy</subject><subject>Average linear density</subject><subject>Brown dwarf stars</subject><subject>Brown dwarfs</subject><subject>Dwarf stars</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Extrasolar planets</subject><subject>Fine structure</subject><subject>Flux density</subject><subject>Forming</subject><subject>Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations</subject><subject>Geometric lines</subject><subject>Interferometers</subject><subject>Interferometry</subject><subject>Low luminosity stars, subdwarfs, and brown dwarfs</subject><subject>Mass</subject><subject>Normal stars (by class): general or individual</subject><subject>Protostars</subject><subject>Radio, microwave (> 1 mm)</subject><subject>Stars</subject><subject>Stellar masses</subject><subject>Sun</subject><issn>0036-8075</issn><issn>1095-9203</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqF0M9LwzAUB_AgipvTsyelIIKXbi8_2xx1_hoM9KDnkqYJdHTNTFqG_72R1QleJId3eJ_3knwROscwxZiIWdC1abWZYkKIAHKAxhgkTyUBeojGAFSkOWR8hE5CWAHEnqTHaERIJjJJ6BjRRdsZb413a9P5WieLyrRdbWututq1ibOJSl69Se-827bJ_VZ5e4qOrGqCORvqBL0_PrzNn9Ply9NifrtMNctEl0puc8WpMBbnpdTM8KwCLImVosJMS6k1VkAqDsxSU9JSl6wSVSlYHh9KBJ2gm93ejXcfvQldsa6DNk2jWuP6UOAc4sFA2f8UCAMphMwivfpDV673bfxIVJTzjOSSRjXbKe1dCN7YYuPrtfKfERXf0RdD9MUQfZy4HPb25dpUe_-TdQTXA1BBq8Z61eo6_DoRrxcMR3exc6vQOb_vM8xzToDTLwzZlAk</recordid><startdate>20120706</startdate><enddate>20120706</enddate><creator>André, Philippe</creator><creator>Ward-Thompson, Derek</creator><creator>Greaves, Jane</creator><general>American Association for the Advancement of Science</general><general>The American Association for the Advancement of Science</general><scope>IQODW</scope><scope>NPM</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7QF</scope><scope>7QG</scope><scope>7QL</scope><scope>7QP</scope><scope>7QQ</scope><scope>7QR</scope><scope>7SC</scope><scope>7SE</scope><scope>7SN</scope><scope>7SP</scope><scope>7SR</scope><scope>7SS</scope><scope>7T7</scope><scope>7TA</scope><scope>7TB</scope><scope>7TK</scope><scope>7TM</scope><scope>7U5</scope><scope>7U9</scope><scope>8BQ</scope><scope>8FD</scope><scope>C1K</scope><scope>F28</scope><scope>FR3</scope><scope>H8D</scope><scope>H8G</scope><scope>H94</scope><scope>JG9</scope><scope>JQ2</scope><scope>K9.</scope><scope>KR7</scope><scope>L7M</scope><scope>L~C</scope><scope>L~D</scope><scope>M7N</scope><scope>P64</scope><scope>RC3</scope><scope>7X8</scope></search><sort><creationdate>20120706</creationdate><title>Interferometric Identification of a Pre-Brown Dwarf</title><author>André, Philippe ; Ward-Thompson, Derek ; Greaves, Jane</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c476t-95f8a536ef18b9c4e57d0192f96d14c99cc1a02d504f3eb3bcb4d6db648009263</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Alps</topic><topic>Astronomical objects</topic><topic>Astronomical observations</topic><topic>Astronomy</topic><topic>Average linear density</topic><topic>Brown dwarf stars</topic><topic>Brown dwarfs</topic><topic>Dwarf stars</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Extrasolar planets</topic><topic>Fine structure</topic><topic>Flux density</topic><topic>Forming</topic><topic>Fundamental astronomy and astrophysics. 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| ispartof | Science (American Association for the Advancement of Science), 2012-07, Vol.337 (6090), p.69-72 |
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| subjects | Alps Astronomical objects Astronomical observations Astronomy Average linear density Brown dwarf stars Brown dwarfs Dwarf stars Earth, ocean, space Exact sciences and technology Extrasolar planets Fine structure Flux density Forming Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations Geometric lines Interferometers Interferometry Low luminosity stars, subdwarfs, and brown dwarfs Mass Normal stars (by class): general or individual Protostars Radio, microwave (> 1 mm) Stars Stellar masses Sun |
| title | Interferometric Identification of a Pre-Brown Dwarf |
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