The 0.1-2.5 keV X-ray spectrum of the O4f star ζ Puppis
We have obtained a high quality ROSAT PSPC spectrum of the bright O4f star Zeta Pup. Allowing for the wind X-ray opacity, as computed from detailed non-LTE stellar wind models of Zeta Pup, and under the assumption that the X-rays arise from shocks distributed throughout the wind, we have been able t...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 1993-09, Vol.276 (1), p.117-128 |
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| container_title | Astronomy and astrophysics (Berlin) |
| container_volume | 276 |
| creator | HILLIER, D. J KUDRITZKI, R. P PAULDRACH, A. W BAADE, D CASSINELLI, J. P PULS, J SCHMITT, J. H. M. M |
| description | We have obtained a high quality ROSAT PSPC spectrum of the bright O4f star Zeta Pup. Allowing for the wind X-ray opacity, as computed from detailed non-LTE stellar wind models of Zeta Pup, and under the assumption that the X-rays arise from shocks distributed throughout the wind, we have been able to match the observed X-ray spectrum (0.1-2.5keV). The best model fit is obtained when He(++) recombines to He(+) in the outer regions of the stellar wind, as predicted by recent detailed cool wind model calculations. With a single temperature plasma, the best model fit indicates a temperature of log Ts(K) = 6.5-6.6, corresponding to shock velocities of around 500 km/s. A 2-temperature plasma yields a significantly improved fit and indicates temperatures of log Ts(K) = 6.2 and 6.7 for the 2 components. The hotter component accounts for 55 percent of the intrinsic (75 percent of the observed) X-ray flux. |
| format | Article |
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J ; KUDRITZKI, R. P ; PAULDRACH, A. W ; BAADE, D ; CASSINELLI, J. P ; PULS, J ; SCHMITT, J. H. M. M</creator><creatorcontrib>HILLIER, D. J ; KUDRITZKI, R. P ; PAULDRACH, A. W ; BAADE, D ; CASSINELLI, J. P ; PULS, J ; SCHMITT, J. H. M. M</creatorcontrib><description>We have obtained a high quality ROSAT PSPC spectrum of the bright O4f star Zeta Pup. Allowing for the wind X-ray opacity, as computed from detailed non-LTE stellar wind models of Zeta Pup, and under the assumption that the X-rays arise from shocks distributed throughout the wind, we have been able to match the observed X-ray spectrum (0.1-2.5keV). The best model fit is obtained when He(++) recombines to He(+) in the outer regions of the stellar wind, as predicted by recent detailed cool wind model calculations. With a single temperature plasma, the best model fit indicates a temperature of log Ts(K) = 6.5-6.6, corresponding to shock velocities of around 500 km/s. A 2-temperature plasma yields a significantly improved fit and indicates temperatures of log Ts(K) = 6.2 and 6.7 for the 2 components. 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With a single temperature plasma, the best model fit indicates a temperature of log Ts(K) = 6.5-6.6, corresponding to shock velocities of around 500 km/s. A 2-temperature plasma yields a significantly improved fit and indicates temperatures of log Ts(K) = 6.2 and 6.7 for the 2 components. 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M</creatorcontrib><collection>Pascal-Francis</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>HILLIER, D. J</au><au>KUDRITZKI, R. P</au><au>PAULDRACH, A. W</au><au>BAADE, D</au><au>CASSINELLI, J. P</au><au>PULS, J</au><au>SCHMITT, J. H. M. M</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The 0.1-2.5 keV X-ray spectrum of the O4f star ζ Puppis</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>1993-09-01</date><risdate>1993</risdate><volume>276</volume><issue>1</issue><spage>117</spage><epage>128</epage><pages>117-128</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><coden>AAEJAF</coden><abstract>We have obtained a high quality ROSAT PSPC spectrum of the bright O4f star Zeta Pup. Allowing for the wind X-ray opacity, as computed from detailed non-LTE stellar wind models of Zeta Pup, and under the assumption that the X-rays arise from shocks distributed throughout the wind, we have been able to match the observed X-ray spectrum (0.1-2.5keV). The best model fit is obtained when He(++) recombines to He(+) in the outer regions of the stellar wind, as predicted by recent detailed cool wind model calculations. With a single temperature plasma, the best model fit indicates a temperature of log Ts(K) = 6.5-6.6, corresponding to shock velocities of around 500 km/s. A 2-temperature plasma yields a significantly improved fit and indicates temperatures of log Ts(K) = 6.2 and 6.7 for the 2 components. The hotter component accounts for 55 percent of the intrinsic (75 percent of the observed) X-ray flux.</abstract><cop>Les Ulis</cop><pub>EDP Sciences</pub><tpages>12</tpages></addata></record> |
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| ispartof | Astronomy and astrophysics (Berlin), 1993-09, Vol.276 (1), p.117-128 |
| issn | 0004-6361 1432-0746 |
| language | eng |
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| source | EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Astronomy Earth, ocean, space Exact sciences and technology Normal stars (by class): general or individual Stars Supergiant stars |
| title | The 0.1-2.5 keV X-ray spectrum of the O4f star ζ Puppis |
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