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THE CIRCUMSTELLAR DISK OF THE Be STAR o AQUARII AS CONSTRAINED BY SIMULTANEOUS SPECTROSCOPY AND OPTICAL INTERFEROMETRY
ABSTRACT Omicron Aquarii is a late-type, Be shell star with a stable and nearly symmetric H emission line. We combine H interferometric observations obtained with the Navy Precision Optical Interferometer covering 2007 through 2014 with H spectroscopic observations over the same period and a 2008 ob...
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Published in: | The Astrophysical journal 2015-12, Vol.814 (2), p.1-12 |
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description | ABSTRACT Omicron Aquarii is a late-type, Be shell star with a stable and nearly symmetric H emission line. We combine H interferometric observations obtained with the Navy Precision Optical Interferometer covering 2007 through 2014 with H spectroscopic observations over the same period and a 2008 observation of the system's near-infrared spectral energy distribution to constrain the properties of o Aqr's circumstellar disk. All observations are consistent with a circumstellar disk seen at an inclination of 75° 3° with a position angle on the sky of 110° 8° measured East from North. From the best-fit disk density model, we find that 90% of the H emission arises from within 9.5 stellar radii, and the mass associated with this H disk is ∼1.8 × 10−10 of the stellar mass, and that the associated angular momentum, assuming Keplerian rotation for the disk, is ∼1.6 × 10−8 of the total stellar angular momentum. The occurrence of a central quasi-emission feature in Mg ii λ4481 is also predicted by this best-fit disk model and the computed profile compares successfully with observations from 1999. To obtain consistency between the H line profile modeling and the other constraints, it was necessary in the profile fitting to weight the line core (emission peaks and central depression) more heavily than the line wings, which were not well reproduced by our models. This may reflect the limitation of assuming a single power law for the disk's variation in equatorial density. The best-fit disk density model for o Aqr predicts that H is near its maximum strength as a function of disk density, and hence the H equivalent width and line profile change only weakly in response to large (factor of ∼5) changes in the disk density. This may in part explain the remarkable observed stability of o Aqr's H emission line profile. |
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A. A. ; Tycner, C. ; Jansen, B. ; Zavala, R. T.</creator><creatorcontrib>Sigut, T. A. A. ; Tycner, C. ; Jansen, B. ; Zavala, R. T.</creatorcontrib><description>ABSTRACT Omicron Aquarii is a late-type, Be shell star with a stable and nearly symmetric H emission line. We combine H interferometric observations obtained with the Navy Precision Optical Interferometer covering 2007 through 2014 with H spectroscopic observations over the same period and a 2008 observation of the system's near-infrared spectral energy distribution to constrain the properties of o Aqr's circumstellar disk. All observations are consistent with a circumstellar disk seen at an inclination of 75° 3° with a position angle on the sky of 110° 8° measured East from North. From the best-fit disk density model, we find that 90% of the H emission arises from within 9.5 stellar radii, and the mass associated with this H disk is ∼1.8 × 10−10 of the stellar mass, and that the associated angular momentum, assuming Keplerian rotation for the disk, is ∼1.6 × 10−8 of the total stellar angular momentum. The occurrence of a central quasi-emission feature in Mg ii λ4481 is also predicted by this best-fit disk model and the computed profile compares successfully with observations from 1999. To obtain consistency between the H line profile modeling and the other constraints, it was necessary in the profile fitting to weight the line core (emission peaks and central depression) more heavily than the line wings, which were not well reproduced by our models. This may reflect the limitation of assuming a single power law for the disk's variation in equatorial density. The best-fit disk density model for o Aqr predicts that H is near its maximum strength as a function of disk density, and hence the H equivalent width and line profile change only weakly in response to large (factor of ∼5) changes in the disk density. This may in part explain the remarkable observed stability of o Aqr's H emission line profile.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/814/2/159</identifier><language>eng</language><publisher>United States: The American Astronomical Society</publisher><subject>Accretion disks ; ANGULAR MOMENTUM ; Aqr ; Aquariums ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; circumstellar matter ; COMPARATIVE EVALUATIONS ; DENSITY ; Disks ; EMISSION SPECTRA ; ENERGY SPECTRA ; HYDROGEN ; INCLINATION ; Interferometers ; INTERFEROMETRY ; MAGNESIUM ; MASS ; Mathematical models ; NEAR INFRARED RADIATION ; ROTATION ; SKY ; Spectroscopy ; STARS ; stars: emission-line, Be ; stars: individual ; techniques: interferometric</subject><ispartof>The Astrophysical journal, 2015-12, Vol.814 (2), p.1-12</ispartof><rights>2015. The American Astronomical Society. All rights reserved.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c383t-a3c41089b78b3e80cdf80362debd9c513ba0e89aa1bd8e5b8bb25e98bd15725f3</citedby><cites>FETCH-LOGICAL-c383t-a3c41089b78b3e80cdf80362debd9c513ba0e89aa1bd8e5b8bb25e98bd15725f3</cites><orcidid>0000-0002-0803-8615</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,315,786,790,891,27957,27958</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22521832$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Sigut, T. A. A.</creatorcontrib><creatorcontrib>Tycner, C.</creatorcontrib><creatorcontrib>Jansen, B.</creatorcontrib><creatorcontrib>Zavala, R. T.</creatorcontrib><title>THE CIRCUMSTELLAR DISK OF THE Be STAR o AQUARII AS CONSTRAINED BY SIMULTANEOUS SPECTROSCOPY AND OPTICAL INTERFEROMETRY</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>ABSTRACT Omicron Aquarii is a late-type, Be shell star with a stable and nearly symmetric H emission line. We combine H interferometric observations obtained with the Navy Precision Optical Interferometer covering 2007 through 2014 with H spectroscopic observations over the same period and a 2008 observation of the system's near-infrared spectral energy distribution to constrain the properties of o Aqr's circumstellar disk. All observations are consistent with a circumstellar disk seen at an inclination of 75° 3° with a position angle on the sky of 110° 8° measured East from North. From the best-fit disk density model, we find that 90% of the H emission arises from within 9.5 stellar radii, and the mass associated with this H disk is ∼1.8 × 10−10 of the stellar mass, and that the associated angular momentum, assuming Keplerian rotation for the disk, is ∼1.6 × 10−8 of the total stellar angular momentum. The occurrence of a central quasi-emission feature in Mg ii λ4481 is also predicted by this best-fit disk model and the computed profile compares successfully with observations from 1999. To obtain consistency between the H line profile modeling and the other constraints, it was necessary in the profile fitting to weight the line core (emission peaks and central depression) more heavily than the line wings, which were not well reproduced by our models. This may reflect the limitation of assuming a single power law for the disk's variation in equatorial density. The best-fit disk density model for o Aqr predicts that H is near its maximum strength as a function of disk density, and hence the H equivalent width and line profile change only weakly in response to large (factor of ∼5) changes in the disk density. This may in part explain the remarkable observed stability of o Aqr's H emission line profile.</description><subject>Accretion disks</subject><subject>ANGULAR MOMENTUM</subject><subject>Aqr</subject><subject>Aquariums</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>circumstellar matter</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>DENSITY</subject><subject>Disks</subject><subject>EMISSION SPECTRA</subject><subject>ENERGY SPECTRA</subject><subject>HYDROGEN</subject><subject>INCLINATION</subject><subject>Interferometers</subject><subject>INTERFEROMETRY</subject><subject>MAGNESIUM</subject><subject>MASS</subject><subject>Mathematical models</subject><subject>NEAR INFRARED RADIATION</subject><subject>ROTATION</subject><subject>SKY</subject><subject>Spectroscopy</subject><subject>STARS</subject><subject>stars: emission-line, Be</subject><subject>stars: individual</subject><subject>techniques: interferometric</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqFkc2O0zAURiMEEmXgCdhYYsMmxD9xYy8zqctEpElJHImurNhxRUadpsQp0rz9OCpiCSvr2ue7kr8TBB8R_IIgYxGEMA7XJPkRMRRHOEKUvwpWiBIWxoQmr4PVX-Jt8M65x2XEnK-C3_JBgCyvs3bXSFEUaQ02efMNVFuwvNxb0Eh_N4L0e5vWeQ7SBmRV2cg6zUuxAfcH0OS7tpBpKaq2Ac1eZLKumqzaH0BabkC1l3mWFiAvpai3oq52QtaH98GbY3dy9sOf8y5ot0JmD2FRfV3w0BBG5rAjJvYf5DphmlgGTX9kkKxxb3XPDUVEd9Ay3nVI98xSzbTG1HKme0QTTI_kLvh02zu6eVDODLM1P814PlszK4wpRoxgT32-UZdp_HW1blZPgzP2dOrOdrw6hRha-74SSP-PJhxy3zmJPUpuqJlG5yZ7VJdpeOqmZ4WgWrSpxYJapCivTWHltflUdEsN40U9jtfp7Pv5Z-IFg2uO0w</recordid><startdate>20151201</startdate><enddate>20151201</enddate><creator>Sigut, T. A. A.</creator><creator>Tycner, C.</creator><creator>Jansen, B.</creator><creator>Zavala, R. T.</creator><general>The American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-0803-8615</orcidid></search><sort><creationdate>20151201</creationdate><title>THE CIRCUMSTELLAR DISK OF THE Be STAR o AQUARII AS CONSTRAINED BY SIMULTANEOUS SPECTROSCOPY AND OPTICAL INTERFEROMETRY</title><author>Sigut, T. A. A. ; Tycner, C. ; Jansen, B. ; Zavala, R. T.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c383t-a3c41089b78b3e80cdf80362debd9c513ba0e89aa1bd8e5b8bb25e98bd15725f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Accretion disks</topic><topic>ANGULAR MOMENTUM</topic><topic>Aqr</topic><topic>Aquariums</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>circumstellar matter</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>DENSITY</topic><topic>Disks</topic><topic>EMISSION SPECTRA</topic><topic>ENERGY SPECTRA</topic><topic>HYDROGEN</topic><topic>INCLINATION</topic><topic>Interferometers</topic><topic>INTERFEROMETRY</topic><topic>MAGNESIUM</topic><topic>MASS</topic><topic>Mathematical models</topic><topic>NEAR INFRARED RADIATION</topic><topic>ROTATION</topic><topic>SKY</topic><topic>Spectroscopy</topic><topic>STARS</topic><topic>stars: emission-line, Be</topic><topic>stars: individual</topic><topic>techniques: interferometric</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Sigut, T. A. A.</creatorcontrib><creatorcontrib>Tycner, C.</creatorcontrib><creatorcontrib>Jansen, B.</creatorcontrib><creatorcontrib>Zavala, R. T.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sigut, T. A. A.</au><au>Tycner, C.</au><au>Jansen, B.</au><au>Zavala, R. T.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>THE CIRCUMSTELLAR DISK OF THE Be STAR o AQUARII AS CONSTRAINED BY SIMULTANEOUS SPECTROSCOPY AND OPTICAL INTERFEROMETRY</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2015-12-01</date><risdate>2015</risdate><volume>814</volume><issue>2</issue><spage>1</spage><epage>12</epage><pages>1-12</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><notes>ApJ99115</notes><notes>Stars</notes><notes>ObjectType-Article-1</notes><notes>SourceType-Scholarly Journals-1</notes><notes>ObjectType-Feature-2</notes><notes>content type line 23</notes><abstract>ABSTRACT Omicron Aquarii is a late-type, Be shell star with a stable and nearly symmetric H emission line. We combine H interferometric observations obtained with the Navy Precision Optical Interferometer covering 2007 through 2014 with H spectroscopic observations over the same period and a 2008 observation of the system's near-infrared spectral energy distribution to constrain the properties of o Aqr's circumstellar disk. All observations are consistent with a circumstellar disk seen at an inclination of 75° 3° with a position angle on the sky of 110° 8° measured East from North. From the best-fit disk density model, we find that 90% of the H emission arises from within 9.5 stellar radii, and the mass associated with this H disk is ∼1.8 × 10−10 of the stellar mass, and that the associated angular momentum, assuming Keplerian rotation for the disk, is ∼1.6 × 10−8 of the total stellar angular momentum. The occurrence of a central quasi-emission feature in Mg ii λ4481 is also predicted by this best-fit disk model and the computed profile compares successfully with observations from 1999. To obtain consistency between the H line profile modeling and the other constraints, it was necessary in the profile fitting to weight the line core (emission peaks and central depression) more heavily than the line wings, which were not well reproduced by our models. This may reflect the limitation of assuming a single power law for the disk's variation in equatorial density. The best-fit disk density model for o Aqr predicts that H is near its maximum strength as a function of disk density, and hence the H equivalent width and line profile change only weakly in response to large (factor of ∼5) changes in the disk density. This may in part explain the remarkable observed stability of o Aqr's H emission line profile.</abstract><cop>United States</cop><pub>The American Astronomical Society</pub><doi>10.1088/0004-637X/814/2/159</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0002-0803-8615</orcidid></addata></record> |
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subjects | Accretion disks ANGULAR MOMENTUM Aqr Aquariums ASTROPHYSICS, COSMOLOGY AND ASTRONOMY circumstellar matter COMPARATIVE EVALUATIONS DENSITY Disks EMISSION SPECTRA ENERGY SPECTRA HYDROGEN INCLINATION Interferometers INTERFEROMETRY MAGNESIUM MASS Mathematical models NEAR INFRARED RADIATION ROTATION SKY Spectroscopy STARS stars: emission-line, Be stars: individual techniques: interferometric |
title | THE CIRCUMSTELLAR DISK OF THE Be STAR o AQUARII AS CONSTRAINED BY SIMULTANEOUS SPECTROSCOPY AND OPTICAL INTERFEROMETRY |
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