Ultraviolet spectroscopy of V Sagittae in high, intermediate and low states from HST and IUE satellites
We present the first phase resolved ultraviolet spectroscopic study of V Sge in high, intermediate and low states observed with the Hubble Space Telescope High Resolution Spectrograph (HST HRS) and International Ultraviolet Explorer (IUE) during the period 1978–1996 to diagnose the ultraviolet fluxe...
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| description | We present the first phase resolved ultraviolet spectroscopic study of V Sge in high, intermediate and low states observed with the Hubble Space Telescope High Resolution Spectrograph (HST HRS) and International Ultraviolet Explorer (IUE) during the period 1978–1996 to diagnose the ultraviolet fluxes of C IV 1550 Å and He II 1640 Å emission lines originating in the accretion disk during different orbital phases. Different spectra showing the variations in line fluxes at different orbital phases are presented. The reddening of V Sge is determined from the 2200 Å feature. We concentrated on calculating the line fluxes of C IV & He II emission lines. From HST and IUE data, we derived an accretion luminosity and an accretion rate for V Sge. The average temperature of the outer rim of the accretion disk
∼
10000
K
. Our results show that there are variations in line fluxes, accretion luminosities and accretion rates with time for V Sge. These variations are attributed to the variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. These results from the HST and IUE observations are consistent with the binary model consisting of a white dwarf, a disk around the white dwarf, and a lobe-filling main-sequence companion (Hachisu & Kato, Astrophys. J. 598:527H,
2003
). |
| doi_str_mv | 10.1007/s10509-015-2542-x |
| format | Article |
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∼
10000
K
. Our results show that there are variations in line fluxes, accretion luminosities and accretion rates with time for V Sge. These variations are attributed to the variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. These results from the HST and IUE observations are consistent with the binary model consisting of a white dwarf, a disk around the white dwarf, and a lobe-filling main-sequence companion (Hachisu & Kato, Astrophys. J. 598:527H,
2003
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∼
10000
K
. Our results show that there are variations in line fluxes, accretion luminosities and accretion rates with time for V Sge. These variations are attributed to the variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. These results from the HST and IUE observations are consistent with the binary model consisting of a white dwarf, a disk around the white dwarf, and a lobe-filling main-sequence companion (Hachisu & Kato, Astrophys. J. 598:527H,
2003
).</description><subject>Accretion</subject><subject>Accretion disks</subject><subject>Astrobiology</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Cosmology</subject><subject>Emissions</subject><subject>Fluxes</subject><subject>IUE</subject><subject>Luminosity</subject><subject>Mass transfer</subject><subject>Observations and Techniques</subject><subject>Orbitals</subject><subject>Original Article</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Ultraviolet</subject><subject>Ultraviolet spectroscopy</subject><subject>White dwarf stars</subject><issn>0004-640X</issn><issn>1572-946X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNqFkUtLAzEUhYMoWB8_wF3AjQtHb5LJZLIU8QWCC1vpLsTMnToyndQk9fHvTa0LEcRVcm--c8i9h5ADBicMQJ1GBhJ0AUwWXJa8eN8gIyYVL3RZTTfJCADKoiphuk12YnzOpa60GpHZpE_Bvna-x0TjAl0KPjq_-KC-pQ_03s66lCzSbqBP3ezpOF8Shjk2nU1I7dDQ3r_RmHIVaRv8nF7fj7_6N5MLGnO777v8tke2WttH3P8-d8n48mJ8fl3c3l3dnJ_dFk6IMhUcBGvrR6Gsa0StGarG8bYtnW4ArEbkeU50vGHAEbjQSqhaVgKZdqIBsUuO1raL4F-WGJOZd9HlP9gB_TIaVuc9aK2l_B9VNUimoVq5Hv5Cn_0yDHmOTJVaal6plSFbUy6vMAZszSJ0cxs-DAOzCsmsQzI5JLMKybxnDV9rYmaHGYYfzn-KPgHfPZQI</recordid><startdate>20151101</startdate><enddate>20151101</enddate><creator>Sanad, M. 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R.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection (ProQuest)</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Astrophysics and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sanad, M. R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Ultraviolet spectroscopy of V Sagittae in high, intermediate and low states from HST and IUE satellites</atitle><jtitle>Astrophysics and space science</jtitle><stitle>Astrophys Space Sci</stitle><date>2015-11-01</date><risdate>2015</risdate><volume>360</volume><issue>1</issue><spage>1</spage><epage>9</epage><pages>1-9</pages><artnum>31</artnum><issn>0004-640X</issn><eissn>1572-946X</eissn><abstract>We present the first phase resolved ultraviolet spectroscopic study of V Sge in high, intermediate and low states observed with the Hubble Space Telescope High Resolution Spectrograph (HST HRS) and International Ultraviolet Explorer (IUE) during the period 1978–1996 to diagnose the ultraviolet fluxes of C IV 1550 Å and He II 1640 Å emission lines originating in the accretion disk during different orbital phases. Different spectra showing the variations in line fluxes at different orbital phases are presented. The reddening of V Sge is determined from the 2200 Å feature. We concentrated on calculating the line fluxes of C IV & He II emission lines. From HST and IUE data, we derived an accretion luminosity and an accretion rate for V Sge. The average temperature of the outer rim of the accretion disk
∼
10000
K
. Our results show that there are variations in line fluxes, accretion luminosities and accretion rates with time for V Sge. These variations are attributed to the variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. These results from the HST and IUE observations are consistent with the binary model consisting of a white dwarf, a disk around the white dwarf, and a lobe-filling main-sequence companion (Hachisu & Kato, Astrophys. J. 598:527H,
2003
).</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s10509-015-2542-x</doi><tpages>9</tpages></addata></record> |
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| subjects | Accretion Accretion disks Astrobiology Astronomy Astrophysics Astrophysics and Astroparticles Cosmology Emissions Fluxes IUE Luminosity Mass transfer Observations and Techniques Orbitals Original Article Physics Physics and Astronomy Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Ultraviolet Ultraviolet spectroscopy White dwarf stars |
| title | Ultraviolet spectroscopy of V Sagittae in high, intermediate and low states from HST and IUE satellites |
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