Results 71 to 80 of about 141,416 (254)
Models for the soft X-ray emission of post-outburst classical novae
, 2005 A hydrostatic and stationary white dwarf envelope model has been developed for the study of the post-outburst phases of classical novae and their soft X-ray emission.
Hernanz, Margarita, Sala, Gloria
core +1 more source
Nuclear Mixing Meters for Classical Novae [PDF]
, 2013 Classical novae are caused by mass transfer episodes from a main sequence star onto a white dwarf via Roche lobe overflow. This material forms an accretion disk around the white dwarf.
Champagne, Art +4 more
core +3 more sources
Reconstruction of the Structure of Accretion Disks in Dwarf Novae from the Multi-Band Light Curves of Early Superhumps [PDF]
, 2012 We propose a new method to reconstruct the structure of accretion disks in dwarf novae using multi-band light curves of early superhumps. Our model assumes that early superhumps are caused by the rotation effect of non-axisymmetrically flaring disks.
M. Uemura +3 more
semanticscholar +1 more source
The Astrophysical Journal, 1983 Observational data on mass-transfer rates and radii of disks indicate that the outer parts of disks in novae and nova-like binaries are sufficiently hot for stationary accretion; those in dwarf novae are too cool to avoid an accretion instability, while these in Z Cam systems are the borderline cases.
openaire +1 more source
Symposium - International Astronomical Union, 1976 Recent work on the physical processes resulting from mass transfer between the red and blue components of dwarf nova binaries is reviewed. The optical behaviour of the blue component's accretion disc suggests that it may be the infall, accretion energy which is being liberated during outbursts.
openaire +1 more source
THE DWARF NOVA OUTBURSTS OF NOVA HER 1960 (=V446 HER) [PDF]
The Astronomical Journal, 2011 To appear at the Astronomical Journal; 7 pages, 1 table, 11 ...
Honeycutt, R. K. +2 more
openaire +2 more sources
V2487 Oph 1998: a post nova in an intermediate polar
EPJ Web of Conferences, 2014 V2487 Oph (Nova Oph 1998) is a classical nova that exploded in 1998. XMM-Newton observations performed between 2 and 9 years after the explosion showed emission related to restablished accretion, and indicative of a magnetic white dwarf.
Hernanz Margarita
doaj +1 more source
A multiwavelength survey of NGC 6752: X-ray counterparts, two new dwarf novae and a core-collapsed radial profile [PDF]
, 2012 We present the results of a multiwavelength (far-ultraviolet to I band) survey of the stellar populations of the globular cluster NGC 6752, using Space Telescope Imaging Spectrograph (STIS), Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3)
G. Thomson +8 more
semanticscholar +1 more source
Observations of Dwarf Novae [PDF]
Symposium - International Astronomical Union, 1976 Spectroscopic and photometric observations relevant to the structure of classical novae, recurrent novae and dwarf novae are collected together. Details are given of optical, infrared, satellite ultraviolet, X-ray and radio observations. Most of these can be understood in terms of the hot spot model of cataclysmic variable stars.
openaire +1 more source
SWSex Stars, Old Novae, and the Evolution of Cataclysmic Variables
Acta Polytechnica CTU Proceedings, 2015 The population of cataclysmic variables with orbital periods right above the period gap are dominated by systems with extremely high mass transfer rates, the so-called SW Sextantis stars.
L. Schmidtobreick, C. Tappert
doaj +1 more source