STIS Coronagraphic Observations of Beta Pictoris
We present new coronagraphic images of Beta Pictoris obtained with the Space Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution images (0.1") clearly detect the circumstellar disk as close as 0.75" to the star, corresponding to a projected radius of 15 AU. The ima...
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| creator | Heap, Sara R Lindler, Don J Lanz, Thierry M Cornett, Robert H Hubeny, Ivan Maran, Stephen P Woodgate, Bruce |
| description | We present new coronagraphic images of Beta Pictoris obtained with the Space
Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution
images (0.1") clearly detect the circumstellar disk as close as 0.75" to the
star, corresponding to a projected radius of 15 AU. The images define the warp
in the disk with greater precision and at closer radii to Beta Pic than do
previous observations. They show that the warp can be modelled by the
projection of two components: the main disk, and a fainter component, which is
inclined to the main component by 4-5 degrees, and which extends only as far as
~4" from the star. We interpret the main component as arising primarily in the
outer disk and the tilted component as defining the inner region of the disk.
The observed properties of the warped inner disk are inconsistent with a
driving force from stellar radiation. However, warping induced by the
gravitational potential of one or more planets is consistent with the data.
Using models of planet-warped disks constructed by Larwood and Papaloizou
(1997), we derive possible masses of the perturbing object. |
| doi_str_mv | 10.48550/arxiv.astro-ph/9911363 |
| format | Article |
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Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution
images (0.1") clearly detect the circumstellar disk as close as 0.75" to the
star, corresponding to a projected radius of 15 AU. The images define the warp
in the disk with greater precision and at closer radii to Beta Pic than do
previous observations. They show that the warp can be modelled by the
projection of two components: the main disk, and a fainter component, which is
inclined to the main component by 4-5 degrees, and which extends only as far as
~4" from the star. We interpret the main component as arising primarily in the
outer disk and the tilted component as defining the inner region of the disk.
The observed properties of the warped inner disk are inconsistent with a
driving force from stellar radiation. However, warping induced by the
gravitational potential of one or more planets is consistent with the data.
Using models of planet-warped disks constructed by Larwood and Papaloizou
(1997), we derive possible masses of the perturbing object.</description><identifier>DOI: 10.48550/arxiv.astro-ph/9911363</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Earth and Planetary Astrophysics ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics</subject><creationdate>1999-11</creationdate><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/astro-ph/9911363$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.1086/309188$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.astro-ph/9911363$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Heap, Sara R</creatorcontrib><creatorcontrib>Lindler, Don J</creatorcontrib><creatorcontrib>Lanz, Thierry M</creatorcontrib><creatorcontrib>Cornett, Robert H</creatorcontrib><creatorcontrib>Hubeny, Ivan</creatorcontrib><creatorcontrib>Maran, Stephen P</creatorcontrib><creatorcontrib>Woodgate, Bruce</creatorcontrib><title>STIS Coronagraphic Observations of Beta Pictoris</title><description>We present new coronagraphic images of Beta Pictoris obtained with the Space
Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution
images (0.1") clearly detect the circumstellar disk as close as 0.75" to the
star, corresponding to a projected radius of 15 AU. The images define the warp
in the disk with greater precision and at closer radii to Beta Pic than do
previous observations. They show that the warp can be modelled by the
projection of two components: the main disk, and a fainter component, which is
inclined to the main component by 4-5 degrees, and which extends only as far as
~4" from the star. We interpret the main component as arising primarily in the
outer disk and the tilted component as defining the inner region of the disk.
The observed properties of the warped inner disk are inconsistent with a
driving force from stellar radiation. However, warping induced by the
gravitational potential of one or more planets is consistent with the data.
Using models of planet-warped disks constructed by Larwood and Papaloizou
(1997), we derive possible masses of the perturbing object.</description><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1999</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA3NNAzsTA1NdBPLKrILNNLLC4pytctyNC3tDQ0NDYz5mQwCA7xDFZwzi_Kz0tML0osyMhMVvBPKk4tKkssyczPK1bIT1NwSi1JVAjITC7JL8os5mFgTUvMKU7lhdLcDKpuriHOHrpgG-ILijJzE4sq48E2xRdkxENtMiZWHQDBRDll</recordid><startdate>19991118</startdate><enddate>19991118</enddate><creator>Heap, Sara R</creator><creator>Lindler, Don J</creator><creator>Lanz, Thierry M</creator><creator>Cornett, Robert H</creator><creator>Hubeny, Ivan</creator><creator>Maran, Stephen P</creator><creator>Woodgate, Bruce</creator><scope>GOX</scope></search><sort><creationdate>19991118</creationdate><title>STIS Coronagraphic Observations of Beta Pictoris</title><author>Heap, Sara R ; Lindler, Don J ; Lanz, Thierry M ; Cornett, Robert H ; Hubeny, Ivan ; Maran, Stephen P ; Woodgate, Bruce</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_astro_ph_99113633</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1999</creationdate><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Heap, Sara R</creatorcontrib><creatorcontrib>Lindler, Don J</creatorcontrib><creatorcontrib>Lanz, Thierry M</creatorcontrib><creatorcontrib>Cornett, Robert H</creatorcontrib><creatorcontrib>Hubeny, Ivan</creatorcontrib><creatorcontrib>Maran, Stephen P</creatorcontrib><creatorcontrib>Woodgate, Bruce</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Heap, Sara R</au><au>Lindler, Don J</au><au>Lanz, Thierry M</au><au>Cornett, Robert H</au><au>Hubeny, Ivan</au><au>Maran, Stephen P</au><au>Woodgate, Bruce</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>STIS Coronagraphic Observations of Beta Pictoris</atitle><date>1999-11-18</date><risdate>1999</risdate><abstract>We present new coronagraphic images of Beta Pictoris obtained with the Space
Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution
images (0.1") clearly detect the circumstellar disk as close as 0.75" to the
star, corresponding to a projected radius of 15 AU. The images define the warp
in the disk with greater precision and at closer radii to Beta Pic than do
previous observations. They show that the warp can be modelled by the
projection of two components: the main disk, and a fainter component, which is
inclined to the main component by 4-5 degrees, and which extends only as far as
~4" from the star. We interpret the main component as arising primarily in the
outer disk and the tilted component as defining the inner region of the disk.
The observed properties of the warped inner disk are inconsistent with a
driving force from stellar radiation. However, warping induced by the
gravitational potential of one or more planets is consistent with the data.
Using models of planet-warped disks constructed by Larwood and Papaloizou
(1997), we derive possible masses of the perturbing object.</abstract><doi>10.48550/arxiv.astro-ph/9911363</doi><oa>free_for_read</oa></addata></record> |
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| language | eng |
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| subjects | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
| title | STIS Coronagraphic Observations of Beta Pictoris |
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