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The investigation of contemporary classical novae
Astronomical and Astrophysical Transactions, 1998Abstract The investigation of five classical novae: N Cyg 1992 = V1974 Cyg, N Aql 1993 = V1419 Aql, N Cas 1993 = V705 Cas, N Aql 1995 and N Cas 1995 is reported in this paper. The identifications of these novae with faint stars in the Palomar Sky Survey were checked. N Aql 1993 was identified with a star of 21 mag on the POSS O plate.
S Yu Shugarov +2 more
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Mixing fraction in classical novae
Astronomy and Astrophysics, 2022 Context. Classical novae are powered by thermonuclear runaways occurring on the surface of accreting white dwarfs (WDs). In the observations, the enrichments of heavy elements in nova ejecta have been detected, indicating a mixing process between the ...
Chengyuan Wu, Yunlang Guo
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The Infrared Temporal Development of Classical Novae
Annual Review of Astronomy and Astrophysics, 1988L'examen des donnees IR existantes concernant les novae permet de decrire les processus physiques qui caracterisent leur developpement post-eruptif, d'identifier les parametres qui distinguent les differents scenarii, de discuter les theories sur l'evolution des systemes binaires serres, de decrire les processus de condensation de la poussiere dans les
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X-ray emission from classical and recurrent novae observed with ROSAT
Astronomy and Astrophysics, 2001 We have analysed 350 pointed and serendipitous observations of 108 different classical and recurrent novae in outburst and in quiescence, contained in the ROSAT archive.
Marina Orio, H Ogelman
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International Astronomical Union Colloquium, 1986
In this review I will present and discuss both the nova outburst and the theoretical calculations related to its cause and evolution. I use the commonly accepted model for a nova: a close binary system with one member a white dwarf and the other member a larger, cooler star that fills its Roche lobe.
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In this review I will present and discuss both the nova outburst and the theoretical calculations related to its cause and evolution. I use the commonly accepted model for a nova: a close binary system with one member a white dwarf and the other member a larger, cooler star that fills its Roche lobe.
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Interacting Winds in Classical Nova Outbursts
Astrophysics and Space Science, 1995Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10-4M⊙of material at velocities of several hundred to a few thousand kilometres ...
Lloyd, H. M. +2 more
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1992
Nova shells are formed from material which is ejected form the surface of a White Dwarf during an outburst. The shells contain usually about 10−5 solar masses and expand with velocities of some hundreds to more than thousand km/s. They reflect the chemical composition of the White Dwarf, the material accreted from the secondary of the binary system ...
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Nova shells are formed from material which is ejected form the surface of a White Dwarf during an outburst. The shells contain usually about 10−5 solar masses and expand with velocities of some hundreds to more than thousand km/s. They reflect the chemical composition of the White Dwarf, the material accreted from the secondary of the binary system ...
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BATSE observations of classical novae
AIP Conference Proceedings, 2000Detection of gamma-ray emission from classical novae, in the range between 30 and 511 keV, would provide a crucial test of the thermonuclear runaway (TNR) model. This emission results from the annihilation of positrons, emitted by some radioactive nuclei (13N and 18F) synthesized during the TNR; it has a short duration and is produced before the ...
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