Электронный архив

Просмотр по теме "Novae, cataclysmic variables"

Просмотр по теме "Novae, cataclysmic variables"

Отсортировать по:Сортировать:Результаты поиска на странице:

  • Soraisam M.; Gilfanov M. (2015)
    © 2015 ESO. With the progenitors of type Ia supernovae (SNe Ia) still eluding direct detections, various types of accreting white dwarfs (WDs) have been proposed as prospective candidates. One of the possibilities are WDs ...
  • Neustroev V.; Suleimanov V.; Borisov N.; Belyakov K.; Shearer A. (2011)
    We present an analysis of time-resolved, medium-resolution optical spectroscopic observations of UX Ursae Majoris (UX UMa) in the blue (3920-5250 Å) and red (6100-7200 Å) wavelength ranges that were obtained in 1999 April ...
  • Suleimanov V.; Doroshenko V.; Ducci L.; Zhukov G.; Werner K. (2016)
    © ESO, 2016.Observed hard X-ray spectra of intermediate polars are determined mainly by the accretion flow velocity at the white dwarf surface, which is normally close to the free-fall velocity. This allows us to estimate ...
  • Korčáková D.; Nagel T.; Werner K.; Suleimanov V.; Votruba V. (2011)
    Context. The velocity field gradient in the radiative transfer in disc models of cataclysmic variables (CVs) is usually neglected; however, the geometry of the system and the value of Keplerian velocity suggest that it can ...
  • Chen H.; Woods T.; Yungelson L.; Gilfanov M.; Han Z. (2016)
    © 2016 The Authors.Theoretical modelling of the evolution of classical and recurrent novae plays an important role in studies of binary evolution, nucleosynthesis and accretion physics. However, from a theoretical perspective ...
  • Неизвестный автор (2018)
    © 2018 ESO. Context. We present more than 4 years of Swift X-ray observations of the 2013 superoutburst, subsequent decline and quiescence of the WZ Sge-type dwarf nova SSS J122221.7-311525 (SSS J122222) from 6 days after ...
  • Kato T.; Dubovsky P.; Kudzej I.; Hambsch F.; Miller I.; Ohshima T.; Nakata C.; Kawabata M.; Nishino H.; Masumoto K.; Mizoguchi S.; Yamanaka M.; Matsumoto K.; Sakai D.; Fukushima D.; Matsuura M.; Bouno G.; Takenaka M.; Nakagawa S.; Noguchi R.; Iino E.; Pickard R.; Maeda Y.; Henden A.; Kasai K.; Kiyota S.; Akazawa H.; Imamura K.; De Miguel E.; Maehara H.; Monard B.; Pavlenko E.; Antonyuk K.; Pit N.; Antonyuk O.; Baklanov A.; Ruiz J.; Richmond M.; Oksanen A.; Harlingten C.; Shugarov S.; Chochol D.; Masi G.; Nocentini F.; Schmeer P.; Bolt G.; Nelson P.; Ulowetz J.; Sabo R.; Goff W.; Stein W.; Michel R.; Dvorak S.; Voloshina I.; Metlov V.; Katysheva N.; Neustroev V.; Sjoberg G.; Littlefield C.; Dębski B.; Sowicka P.; Klimaszewski M.; Curyło M.; Morelle E.; Curtis I.; Iwamatsu H.; Butterworth N.; Andreev M.; Parakhin N.; Sklyanov A.; Shiokawa K.; Novák R.; Irsmambetova T.; Itoh H.; Ito Y.; Hirosawa K.; Denisenko D.; Kochanek C.; Shappee B.; Stanek K.; Prieto J.; Itagaki K.; Stubbings R. (2014)
    © The Author 2014. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved. Continuing the project undertaken by Kato et al. (2009), we collected times of superhump maxima ...

Поиск в электронном архиве

Просмотр

Моя учетная запись