Results 11 to 20 of about 4,008 (285)
Classical and Recurrent Nova Models [PDF]
Proceedings of the International Astronomical Union, 2011 AbstractRemarkable progress in the understanding of nova outbursts has been achieved through combined efforts in photometry, spectroscopy and numerical simulations. According to the thermonuclear runaway model, novae are powered by thermonuclear explosions in the hydrogen-rich envelopes transferred from a low-mass stellar companion onto a close white ...
José Pont, Jordi +5 more
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SHORTEST RECURRENCE PERIODS OF NOVAE [PDF]
The Astrophysical Journal, 2014 8 pages, 9 figures, to appear in ApJ, accepted ...
Mariko Kato +3 more
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The Astrophysical Journal Supplement Series, 2023 M87 has been monitored with a cadence of 5 days over a span of 9 months through the near-ultraviolet (NUV; F275W) and optical (F606W) filters of the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope.
Michael M. Shara +12 more
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THE NOVA SHELL AND EVOLUTION OF THE RECURRENT NOVA T PYXIDIS [PDF]
The Astrophysical Journal, 2009 T Pyxidis is the prototypical recurrent nova (RN) with a mysterious nova shell. We report new observations of the shell with HST. The knots in the shell are expanding with velocities 500-715 km/s, for a distance of 3500 pc. The fractional expansion of the knots is constant, and this implies no significant deceleration.
Schaefer, Bradley E. +2 more
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Theory of Nova Outbursts and Type Ia Supernovae
Acta Polytechnica CTU Proceedings, 2015 We briefly review the current theoretical understanding of the light curves of novae. These curves exhibit a homologous nature, dubbed the universal decline law, and when time-normalized, they almost follow a single curve independently of the white dwarf
M. Kato, I. Hachisu
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International Astronomical Union Colloquium, 1990 AbstractThermonuclear models of recurrent novae demand white dwarf accretors near the Chandrasekhar mass. In this case, the known recurrent novae should possess classical counterparts bearing the same structural parameters and space distribution, save for having only marginally less massive white dwarfs.
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Odessa Astronomical Publications, 2007 The WZ Sge type stars is a rare subclass of the cataclysmic variables (CVs). It possesses the properties of both dwarf novae and recurrent novae. The WZ Sge stars have the shortest orbital periods (typically 80 - 90 minutes) known among the dwarf novae ...
E. P. Pavlenko
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Evidence for Multiple Shocks from the γ-Ray Emission of RS Ophiuchi
The Astrophysical Journal, 2023 In 2021 August, the Fermi Large Area Telescope, H.E.S.S., and MAGIC detected GeV and TeV γ -ray emission from an outburst of recurrent nova RS Ophiuchi. This detection represents the first very high-energy γ -rays observed from a nova, and it opens a new
Rebecca Diesing +6 more
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The nova KT Eri Is a recurrent nova with a recurrence time-scale of 40–50 yr
Monthly Notices of the Royal Astronomical Society, 2022 ABSTRACT KT Eridani was a very fast nova in 2009 peaking at V = 5.42 mag. We marshal large data sets of photometry to finally work out the nature of KT Eri. From the TESS light curve, as confirmed with our radial velocity curve, we find an orbital period of 2.61595 d.
Bradley E Schaefer +3 more
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A pre-outburst signal in the long-term optical light curve of the recurrent nova RS Ophiuchi [PDF]
, 2011 Recurrent novae are binary stars in which a white dwarf accretes matter from a less evolved companion, either a red giant or a main-sequence star. They have dramatic optical brightenings of around 5–6 mag in V in less than a day, several times a century.
A. Sarkar +23 more
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