MARC Record from harvard_bibliographic_metadata

LEADER: 03045nam a22004335a 4500
001 013835667-X
005 20131206200641.0
008 130125s2001 ne | s ||0| 0|eng d
020 $a9789401596886
020 $a9789401596886
020 $a9789048157587
024 7 $a10.1007/978-94-015-9688-6$2doi
035 $a(Springer)9789401596886
040 $aSpringer
050 4 $aQB4
072 7 $aPG$2bicssc
072 7 $aSCI004000$2bisacsh
072 7 $aNAT033000$2bisacsh
082 04 $a520$223
100 1 $aSzczerba, Ryszard,$eeditor.
245 10 $aPost-AGB Objects as a Phase of Stellar Evolution :$bProceedings of the Toruń Workshop held July 5–7, 2000 /$cedited by Ryszard Szczerba, Sławomir K. Górny.
246 3 $aProceedings of the Torun Workshop held July 5-7, 2000
264 1 $aDordrecht :$bSpringer Netherlands :$bImprint: Springer,$c2001.
300 $aXXI, 448 p.$bonline resource.
336 $atext$btxt$2rdacontent
337 $acomputer$bc$2rdamedia
338 $aonline resource$bcr$2rdacarrier
347 $atext file$bPDF$2rda
490 1 $aAstrophysics and Space Science Library,$x0067-0057 ;$v265
520 $aThe term proto-planetary nebulae (PPNe), in the context of the late stages of stellar evolution, was created just over 20 years ago, to express the belief that in the near future these objects will become planetary nebulae (PNe). The first proto-planetary nebulae (also called post-Asymptotic Giant Branch or post-AGB objects) were discovered in the mid-1970s in the course of the Air Force Sky Survey. Investigation of this phase of stellar evolution developed very rapidly in the 1980s after the IRAS mission when it became clear that proto-planetary nebulae emit a significant part of their energy in the mid- and far-infrared. A new impetus in this field began in the 1990s with high spatial resolution imaging in mid-infrared and optical wavelengths. Evidence has been found that proto-planetary nebulae (at least their central parts) are quite asymmetric while shells of AGB stars display spherical shapes. The most intriguing challenge now is to understand which physical processes are dominant during formation and evolution of proto-planetary nebulae. Is it magnetic field, evolution in binary systems, planets, axisymmetric superwind mass loss and its further shaping by fast wind, collimated jets interacting with a spherically symmetric AGB remnant or maybe an interplay between these different processes? Another challenge is to explain why the mass loss process near the end of the AGB evolution is modulated on timescales of a few hundred years. The model presented during this workshop seems to be very promising in this respect.
650 10 $aPhysics.
650 0 $aPhysics.
650 24 $aAstronomy, Observations and Techniques.
650 24 $aAstrophysics and Astroparticles.
700 1 $aGórny, Sławomir K.,$eeditor.
776 08 $iPrinted edition:$z9789048157587
830 0 $aAstrophysics and Space Science Library ;$v265.
988 $a20131114
906 $0VEN