Spectrophotometry of the recently discovered cataclysmic variable CPD -48  1577

Wargau, W.; Drechsel, J.; Rahe, J.; Bruch, A.

doi:10.1093/mnras/204.1.35p

Cited by 18 publications

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“…HAUG index in the far UV range is considerably larger for the higher inclined systems CPD-48°1577 (i»60°; Wargau et al, 1983) and V3885 Sgr (60° < i < 80°; Haug and Drechsel, 1985) than for the lower inclined system RW Sex (25° < i < 30°, Cowley et al, 1977).' The observed wide-range variations of the UV to IR spectral indices lie well within the range of optically thick and stationary accretion disk spectra (see Pigs.…”

Section: Balmer Line Profilessupporting

confidence: 54%

“…The novalike systems CPD-48°1577, V3885 Sgr and RW Sex are the brightest members of the UX UMa-subclass of cataclysmic binaries and are studied since 1968 (for a review, see Wargau et al, 1983;Haug and Drechsel, 1985;Greenstein and Oke, 1982;and references therein). Only recently, PHL 227 {0^=^.6) was discovered by Hunger et al (1985) to exhibit UV and optical spectral behavior very similar to that of V3885 Sgr, though its binary nature has not yet been proven.…”

Section: Introductionmentioning

confidence: 99%

“…The UV spectra SWP 18578 and LWR 14655 of CPD-48°1577 were retrieved from the VILSPA data archive. Part of the optical spectra of CPD-48°1577 and the spectroscopic and photometric data of PHL 227 were taken from measurements published by Wargau et al (1983) and Hunger et al (1985)-UBV photometric data of CPD-48°1577 and IR-JHK measurements of V3885 Sgr are from Bruch (1984) and Epchtein (1985). K. HAUG trie data amount to 0 m .02 and CP-.C5", respectively.…”

Section: Introductionmentioning

confidence: 99%

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Continuum Distributions and Line Profiles of UX UMa-Type Novalike Systems

Haug

1987

International Astronomical Union Colloquium

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ABSTRACT. Combined UV, optical and, in part, IR continuum distributions of the UX UMa-systems CPD-48°1577, V3885 Sgr, RV Sex and of the recently discovered cataclysmic system PHL 227 were determined from multi-wavelength spectroscopic and photometric data to search for general characteristics of these systems. The observed variations of the UV to IR spectral indices are qualitatively very similar for all systems, whereas the absolute values show significant differences in the far and near UV ranges. The wavelength dependence of the optical and IR spectral indices as well as the variations of the Balmer line profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.Based on observations collected at the European Southern Observatory, La Silla, Chile, and with the International Ultraviolet Explorer Satellite at the Villafanca ground station.

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Section: Balmer Line Profilessupporting

confidence: 54%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Continuum Distributions and Line Profiles of UX UMa-Type Novalike Systems

Haug

1987

International Astronomical Union Colloquium

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“…Figure 13 presents a detail of Figure 12, showing a portion of the Balmer series. The gray line is an optical spectrum by Wargau et al (1983). We used the curve-following feature of the ADS Dexter facility to extract the plot from the original publication.…”

Section: The Rim T Eff and The Final System Modelmentioning

confidence: 99%

A Synthetic Spectrum and Light‐Curve Analysis of the Cataclysmic Variable IX Velorum

Linnell¹,

Godon²,

Hubený³

et al. 2007

ApJ

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Spectrum synthesis analysis of F USE and ST IS spectra for the cataclysmic variable IX Vel shows that it is possible to achieve a close synthetic spectrum fit with a mass transfer rate ofṀ = 5×10 −9 M ⊙ /yr −1 and a modified standard model temperature profile. The innermost four annuli of the accretion disk model, extending to r/r wd ≈4, are isothermal; beyond that limit the temperatures follow the standard model.A light synthesis fit to K band photometry requires shallow eclipses of the accretion disk rim and secondary star limb. The geometry constrains the orbital inclination to i = 57±2 • . The synthetic light curve requires a vertically extended accretion disk rim, beyond that predicted by gravitational equilibrium, to shadow

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“…The data so collected refer to the stationary state and hence can serve to find the accretion rate in this phase. These nova-like systems were studied in great detail since 1965 and reviews axe given by Wargau et al 1983, Haug and Drechsel 1985, Greenstein and Oke 1982 To simplify the discussion here we adopt all the parameters of the systems as tabulated by Haug except for the accretion rate. We did not try at this stage to reiterate the parameters and improve the fit beyond the one obtained here.…”

Section: O M P a R I S O N W I T H O B S E R V A T I O N S And R E mentioning

confidence: 99%

The Continuum Spectra of Accretion Discs in Novalike Objects

Shaviv

Wehrsě²

1990

International Astronomical Union Colloquium

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I n t r o d u c t i o nThe exact value of the accretion rate in novae is very important to the theory of thermonuclear runaways and nova statistics. Estimates of the typical accretion rates in nova and novalike objects are 10 1 8 g/s (1.6 10~8 M 0 / y r ) . Patterson (1984) estimated that if the above high accretion rate prevails the expected number of novae according to Bath and Shaviv (1976) exceeds the observed number. Prialnik, Livio, Shaviv and Kovetz (1982) have shown that no thermonuclear runaway can be obtained if the accretion rate is as high as few 1 0 -9 MQ/YI. Actually, the very strong thermonuclear runaways (TNRs) are obtained only for very low accretion rates namely, 1 0 -1 0 to l O _ 1 1 M 0 / y r . A way out from this inconsistency was suggested by Shara, Livio, Moffat and Orio (1986) in the form of the hibernation model. In this model the high accretion rate is found only shortly before and soon after the nuclear runaway and the nova spends most of the time in a state of very low accretion rate -so low that most novae are not observed at all. The high accretion rate, according to this theory, is a precursor to the runaway. The hibernation model is very attractive in spite of a meager observational proof so far and theoretical justifications. Yet, it is one of the most promising ideas in this field. The hibernation scenario claims that the accretion rate is a function of time. It is high just prior to the runaway and it continues to be high for some time just after the runaway. It then declines to very low values. From the point of the model for the thermonuclear runaway the problem is how the star reacts to a temporary high accretion rate that comes after a long period of low accretion rate (Shaviv and Starrfield, 1987). Thus, even if the accretion rate is low during most of the time the phase of high accretion can still affect the outcome of the thermonuclear runaway. The crucial question from the hibernation and T N R point of view is how much mass is accreted with a very low accretion rate and how much mass is accreted during the episode of high accretion. If most of the mass is accreted at high accretion rate hibernation does not help to resolve the problems the theory of T N R has with the high accretion phase. It is therefore important to find the accurate accretion rate in nova and novalike objects. The purpose of this paper is to discuss the accretion rates in novalike objects. There are several observational results for novalike objects that allow us today to evaluate quite accurately the accretion rates from the continuum energy distribution of the accretion disc.The organization of this paper is as follows: since the meeting is dedicated to novae and not to accretion discs and the time alloted to each speaker is short, we will first present the results and the implications and leave the discussion to the end.of use, available at https://www.cambridge.org/core/terms. https://doi

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Spectrophotometry of the recently discovered cataclysmic variable CPD -48 1577

Cited by 18 publications

References 0 publications

Continuum Distributions and Line Profiles of UX UMa-Type Novalike Systems

Continuum Distributions and Line Profiles of UX UMa-Type Novalike Systems

A Synthetic Spectrum and Light‐Curve Analysis of the Cataclysmic Variable IX Velorum

The Continuum Spectra of Accretion Discs in Novalike Objects

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