Infrared Emission of Novae

Geisel, Susan L.; Kleinmann, D. E.; Low, F. J.

doi:10.1086/180579

Cited by 102 publications

(53 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our models with enhanced 12 C and 16 O ejected 10 28 to 10 29 g moving with speeds of 200 to 4000 kms" 1 , kinetic energies of 10 45 erg. In addition, these same models produced total energies of 10 46 to 10 47 erg in excellent agreement with the UV observations (Gallagher and Code, 1974) and the IR observations (Geisel et al, 1970) of FHSer. Those models with no nuclear enhancement (above solar) did not eject any material and their peak kinetic energy, 10 42 erg, was insufficient to eject the ring of material surrounding the white dwarf.…”

Section: Introductionsupporting

confidence: 79%

“…Up to the present time we have used envelope masses of 10" 3 M Q justifying this amount by the work of Giannone and Weigert (1967). In the future, since we are studying white dwarfs with larger masses, we shall reduce the envelope mass to 1 (T 4 M® or less.…”

Section: Hydrostatic Studies Of Accretion Onto White Dwarfsmentioning

confidence: 99%

“…Our modern theoretical studies of the nova outburst date from the work of Giannone and Weigert (1967) who evolved a 0.5 Af© white dwarf accreting hydrogen rich material and showed that a thermonuclear runaway could be initiated in the envelope. Their work was followed by Rose (1968), Redkoborodyi (1972), andTaam andFaulkner (1975).…”

Section: Hydrostatic Studies Of Accretion Onto White Dwarfsmentioning

confidence: 99%

“…As the inflow proceeds the deeper regions are compressed and heated until thermo nuclear temperatures are reached and nuclear burning begins. The original hydrostatic study of accretion onto a white dwarf was discussed by Giannone and Weigert (1967) and Rose (1968) who found that a white dwarf could accrete 10" 3 Af© before the energygeneration time scale had decreased below the mass accretion time scale. Aside from minor variations in the envelope mass, 10" 3 M© is the value that we have used in all our published studies.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The Cause of the Nova Outburst

Starrfield

Sparks

Truran³

1976

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

erg. The theoretical light curves are similar to the observed light curves of common novae during the early stages of the outburst. As a consequence of our studies, we can present an explanation for the continuous ejection of mass which is observed for long times after the initial outburst and for the relationship between maximum magnitude and the decline to minimum. We are also now able to present an explanation for the constant luminosity phase of the outburst and the oval shapes of the ejected nebulae.We have extended our earlier work to models with extreme enhancements of 12 C and to models which include the infalling material in the evolution. The extreme 12 C studies result in outbursts which reach near supernova proportions while the accretion models result in light curves which resemble observed light curves quite closely. Finally, the accretion studies also demonstrate the need for en hanced abundances.

show abstract

Section: Introductionsupporting

confidence: 79%

Section: Hydrostatic Studies Of Accretion Onto White Dwarfsmentioning

confidence: 99%

Section: Hydrostatic Studies Of Accretion Onto White Dwarfsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Cause of the Nova Outburst

Starrfield

Sparks

Truran³

1976

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

show abstract

“…Infrared data for only a few of these objects exist in the literature (Woolf 1969;Geisel, Kleinmann, and Low 1970;Gillett, Merrill, and Stein 1971;Humphreys, Strecker, and Ney 1972). In this paper we present photometric measurements and discuss the origin of the infrared continuum of these stars.…”

Section: Introductionmentioning

confidence: 95%

Photometry of Symbiotic and VV Cephei Stars in the Near Infrared (With a Note on MWC 56)

Swings¹,

Allen²

1972

PASP

View full text Add to dashboard Cite

The majority of symbiotic and VV Cephei stars have near infrared continua closely resembling those of late-type stars. Evidence for weak infrared excesses has been found in the three stars RY Set, W Cep, and U Lac. RX Pup and V1016 Cyg exhibit very prominent infrared excesses which are attributable to thermal radiation from circumstellar dust.The "Rep" star MWC 56, whose spectrum shows Fen and [Fen] emission lines in the blue, possesses the absorption lines of a G or K component in the red. No substantial infrared excess is present.

show abstract

On linear light polarization of novae: dust envelopes

Kučinskas

1990

Astron Nachr

View full text Add to dashboard Cite

Infrared Emission of Novae

Cited by 102 publications

References 0 publications

The Cause of the Nova Outburst

The Cause of the Nova Outburst

Photometry of Symbiotic and VV Cephei Stars in the Near Infrared (With a Note on MWC 56)

On linear light polarization of novae: dust envelopes

Contact Info

Product

Resources

About