MARC Record from marc_columbia

LEADER: 03330cam a2200349Ka 4500
001 6881031
005 20221122055312.0
008 080808s2008 caua f 101 0 eng d
020 $a9781583816547
020 $a1583816542
029 1 $aNLGGC$b314346562
035 $a(OCoLC)ocn241291721
035 $a(OCoLC)241291721
035 $a(NNC)6881031
035 $a6881031
040 $aRAO$cRAO$dYDXCP$dBTCTA$dOrLoB-B
050 0 $aQB 843 .H68 2008
245 00 $aHot subdwarf stars and related objects :$bproceedings of a workshop held at Otto-Friedrich-Universitat, Bamberg, Germany, 23-27 July, 2007 /$cedited by Ulrich Heber, Simon Jeffery, and Ralf Napiwotzki.
260 $aSan Francisco, Calif. :$bAstronomical Society of the Pacific,$c2008.
300 $axv, 386 pages :$billustrations ;$c24 cm.
336 $atext$btxt$2rdacontent
337 $aunmediated$bn$2rdamedia
490 1 $aAstronomical Society of the Pacific (ASP) conference series ;$v392
504 $aIncludes author index, pp. 385-386.
505 00 $gPt. 1.$tHot Subdwarfs in Galaxies and Globular Clusters -- $gPt. 2.$tAtmospheres and Evolution -- $gPt. 3.$tBinaries -- $gPt. 4.$tPulsating sdB/O Stars -- $gPt. 5.$tConference Summary.
520 1 $a"These are the proceedings of the third international workshop on Hot Subdwarf Stars and Related Objects, held in the historic city of Bamberg, Germany, in July 2007." "Hot subdwarfs represent several stages in the very late evolution of low-mass stars. B-type subdwarfs are helium-core burners at the extreme end of the horizontal branch, while O types represent a rich mixture of post-giant branch, post-horizontal branch and post-asymptotic giant branch stars. They are important for many fields of modern astrophysics. Hot subdwarfstars provide: the UV light of old unresolved populations, such as giant elliptical galaxies, wich may be used to measure their ages; laboratories to study plasma processes in high-gravity atmospheres, including radiatively-driven atomic diffusion and its consequences for the chemical composition ofthe star's outer layers; laboratories to study close binary evolution. Many have invisible companions, mostly white dwarfs or low-mass main-sequence stars. Some may have been formed from white-dwarf mergers, while one has a planet, and others may have neutron-star or black-hole companions; laboratories for asteroseismology. Pulsations check the evolution models by giving direct measurements of mass and radius, and the potential to explore other internal properties." "New instruments and theoretical models, as well as a vibrant young research community, are forcing rapid progress in all of these areas. These proceedings provide an informative snapshot of current research. They also include a small number of papers which have been extended to include an introduction for nonspecialists. These papers offer a valuable resource useful to a wide audience including beginning graduate students and experienced reviewers for several years to come."--BOOK JACKET.
650 0 $aDwarf stars$vCongresses.
700 1 $aHeber, Ulrich.
700 1 $aJeffery, C. Simon.
700 1 $aNapiwotzki, Ralf.$0http://id.loc.gov/authorities/names/no2007128152
830 0 $aAstronomical Society of the Pacific (ASP) conference series ;$v392.
852 00 $boff,sci$hQB843$i.H68 2008g