Abundant Crystalline Silicates in the Disk of a Very Low Mass Star
We announce the discovery of SST-Lup3-1, a very low mass star close to the brown dwarf boundary in Lupus III with a circum(sub)stellar disk, discovered by the "Cores to Disks" Spitzer Legacy Program from mid-infrared, with very conspicuous crystalline silicate features in its spectrum. It...
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| Veröffentlicht in: | The Astrophysical journal 2007-05, Vol.661 (1), p.361-367 |
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| creator | Merín, B Augereau, J.-C van Dishoeck, E. F Kessler-Silacci, J Dullemond, C. P Blake, G. A Lahuis, F Brown, J. M Geers, V. C Pontoppidan, K. M Comerón, F Frasca, A Guieu, S Alcalá, J. M Boogert, A. C. A Evans II, N. J D’Alessio, P Mundy, L. G Chapman, N |
| description | We announce the discovery of SST-Lup3-1, a very low mass star close to the brown dwarf boundary in Lupus III with a circum(sub)stellar disk, discovered by the "Cores to Disks" Spitzer Legacy Program from mid-infrared, with very conspicuous crystalline silicate features in its spectrum. It is the first of such objects with a full 5-35 mu m spectrum taken with the IRS, and it shows strong 10 and 20 mu m silicate features with high feature-to-continuum ratios and clear crystalline features out to 33 mu m. The dust in the disk upper layer has a crystalline silicate grain fraction between 15% and 33%, depending on the assumed dust continuum. The availability of the full Spitzer infrared spectrum allows an analysis of the dust composition as a function of temperature and position in the disk. The hot ( similar to 300 K) dust responsible for the 10 mu m feature consists of a roughly equal mix of small ( similar to 0.1 mu m) and large ( similar to 1.5 mu m) grains, whereas the cold ( similar to 70 K) dust responsible for the longer wavelength silicate features contains primarily large grains (>1 mu m). Since the cold dust emission arises from deeper layers in the inner ( |
| doi_str_mv | 10.1086/513092 |
| format | Article |
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F ; Kessler-Silacci, J ; Dullemond, C. P ; Blake, G. A ; Lahuis, F ; Brown, J. M ; Geers, V. C ; Pontoppidan, K. M ; Comerón, F ; Frasca, A ; Guieu, S ; Alcalá, J. M ; Boogert, A. C. A ; Evans II, N. J ; D’Alessio, P ; Mundy, L. G ; Chapman, N</creator><creatorcontrib>Merín, B ; Augereau, J.-C ; van Dishoeck, E. F ; Kessler-Silacci, J ; Dullemond, C. P ; Blake, G. A ; Lahuis, F ; Brown, J. M ; Geers, V. C ; Pontoppidan, K. M ; Comerón, F ; Frasca, A ; Guieu, S ; Alcalá, J. M ; Boogert, A. C. A ; Evans II, N. J ; D’Alessio, P ; Mundy, L. G ; Chapman, N</creatorcontrib><description>We announce the discovery of SST-Lup3-1, a very low mass star close to the brown dwarf boundary in Lupus III with a circum(sub)stellar disk, discovered by the "Cores to Disks" Spitzer Legacy Program from mid-infrared, with very conspicuous crystalline silicate features in its spectrum. It is the first of such objects with a full 5-35 mu m spectrum taken with the IRS, and it shows strong 10 and 20 mu m silicate features with high feature-to-continuum ratios and clear crystalline features out to 33 mu m. The dust in the disk upper layer has a crystalline silicate grain fraction between 15% and 33%, depending on the assumed dust continuum. The availability of the full Spitzer infrared spectrum allows an analysis of the dust composition as a function of temperature and position in the disk. The hot ( similar to 300 K) dust responsible for the 10 mu m feature consists of a roughly equal mix of small ( similar to 0.1 mu m) and large ( similar to 1.5 mu m) grains, whereas the cold ( similar to 70 K) dust responsible for the longer wavelength silicate features contains primarily large grains (>1 mu m). Since the cold dust emission arises from deeper layers in the inner (<3 AU) disk as well as from the surface layers of the outer (3-5 AU) disk, this provides direct evidence for combined grain growth and settling in the disk. The inferred crystalline mass fractions in the two components are comparable. 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F</creatorcontrib><creatorcontrib>Kessler-Silacci, J</creatorcontrib><creatorcontrib>Dullemond, C. P</creatorcontrib><creatorcontrib>Blake, G. A</creatorcontrib><creatorcontrib>Lahuis, F</creatorcontrib><creatorcontrib>Brown, J. M</creatorcontrib><creatorcontrib>Geers, V. C</creatorcontrib><creatorcontrib>Pontoppidan, K. M</creatorcontrib><creatorcontrib>Comerón, F</creatorcontrib><creatorcontrib>Frasca, A</creatorcontrib><creatorcontrib>Guieu, S</creatorcontrib><creatorcontrib>Alcalá, J. M</creatorcontrib><creatorcontrib>Boogert, A. C. A</creatorcontrib><creatorcontrib>Evans II, N. J</creatorcontrib><creatorcontrib>D’Alessio, P</creatorcontrib><creatorcontrib>Mundy, L. G</creatorcontrib><creatorcontrib>Chapman, N</creatorcontrib><title>Abundant Crystalline Silicates in the Disk of a Very Low Mass Star</title><title>The Astrophysical journal</title><description>We announce the discovery of SST-Lup3-1, a very low mass star close to the brown dwarf boundary in Lupus III with a circum(sub)stellar disk, discovered by the "Cores to Disks" Spitzer Legacy Program from mid-infrared, with very conspicuous crystalline silicate features in its spectrum. It is the first of such objects with a full 5-35 mu m spectrum taken with the IRS, and it shows strong 10 and 20 mu m silicate features with high feature-to-continuum ratios and clear crystalline features out to 33 mu m. The dust in the disk upper layer has a crystalline silicate grain fraction between 15% and 33%, depending on the assumed dust continuum. The availability of the full Spitzer infrared spectrum allows an analysis of the dust composition as a function of temperature and position in the disk. The hot ( similar to 300 K) dust responsible for the 10 mu m feature consists of a roughly equal mix of small ( similar to 0.1 mu m) and large ( similar to 1.5 mu m) grains, whereas the cold ( similar to 70 K) dust responsible for the longer wavelength silicate features contains primarily large grains (>1 mu m). Since the cold dust emission arises from deeper layers in the inner (<3 AU) disk as well as from the surface layers of the outer (3-5 AU) disk, this provides direct evidence for combined grain growth and settling in the disk. The inferred crystalline mass fractions in the two components are comparable. 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A</au><au>Evans II, N. J</au><au>D’Alessio, P</au><au>Mundy, L. G</au><au>Chapman, N</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Abundant Crystalline Silicates in the Disk of a Very Low Mass Star</atitle><jtitle>The Astrophysical journal</jtitle><date>2007-05-20</date><risdate>2007</risdate><volume>661</volume><issue>1</issue><spage>361</spage><epage>367</epage><pages>361-367</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>We announce the discovery of SST-Lup3-1, a very low mass star close to the brown dwarf boundary in Lupus III with a circum(sub)stellar disk, discovered by the "Cores to Disks" Spitzer Legacy Program from mid-infrared, with very conspicuous crystalline silicate features in its spectrum. It is the first of such objects with a full 5-35 mu m spectrum taken with the IRS, and it shows strong 10 and 20 mu m silicate features with high feature-to-continuum ratios and clear crystalline features out to 33 mu m. The dust in the disk upper layer has a crystalline silicate grain fraction between 15% and 33%, depending on the assumed dust continuum. The availability of the full Spitzer infrared spectrum allows an analysis of the dust composition as a function of temperature and position in the disk. The hot ( similar to 300 K) dust responsible for the 10 mu m feature consists of a roughly equal mix of small ( similar to 0.1 mu m) and large ( similar to 1.5 mu m) grains, whereas the cold ( similar to 70 K) dust responsible for the longer wavelength silicate features contains primarily large grains (>1 mu m). Since the cold dust emission arises from deeper layers in the inner (<3 AU) disk as well as from the surface layers of the outer (3-5 AU) disk, this provides direct evidence for combined grain growth and settling in the disk. The inferred crystalline mass fractions in the two components are comparable. Since only the inner 0.02 AU of the disk is warm enough to anneal the amorphous silicate grains, even the lowest fraction of 15% of crystalline material requires either very efficient mixing or other formation mechanisms.</abstract><cop>Chicago, IL</cop><pub>IOP Publishing</pub><doi>10.1086/513092</doi><tpages>7</tpages><orcidid>https://orcid.org/0000-0002-0474-0896</orcidid><oa>free_for_read</oa></addata></record> |
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| title | Abundant Crystalline Silicates in the Disk of a Very Low Mass Star |
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