Spectroscopy and orbital periods of the old novae V533 Herculis, V446 Herculis and X Serpentis

Thorstensen, J. R.; Taylor, Charles H.

doi:10.1046/j.1365-8711.2000.03230.x

Cited by 52 publications

(56 citation statements)

References 29 publications

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“…For our Fig. 2 we used the values from their Table 4. A119, page 4 of 24 A remarkable change from α = 0.5 in their 1997 spectrum to α = 1.1 in the spectrum obtained in 1999 was reported by Thorstensen & Taylor (2000).…”

Section: Interstellar Extinction and Spectral Energy Distribution (Sed)mentioning

confidence: 86%

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SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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Aims. We report on recent optical observations of the stellar and the nebular remnants of 22 southern post-novae. Methods. In this study, for each of our targets, we obtained and analysed long-slit spectra in the spectral range 3500-6600 Å and inResults. The changes in the emission lines' equivalent widths with the time since the outburst agree with earlier published results of other authors. We estimated an average value α = 2.37 for the exponent of the power law fitted to the post-novae continua. Our observations clearly show the two-component structure of the V842 Cen expanding nebulae, owing to the different velocities of the ejected matter. We discovered an expanding shell around V382 Vel with an outer diameter of about 12 .

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Section: Interstellar Extinction and Spectral Energy Distribution (Sed)mentioning

confidence: 86%

“…Spectral observations during the X Ser outburst are missing. The numerous published spectra of the remnant (Williams 1983;Shara et al 1986;Duerbeck & Seitter 1990;Szkody & Howell 1992;Ringwald et al 1996;Thorstensen & Taylor 2000) are evidence of remarkable changes in the continuum and the spectral lines.…”

Section: Cn Velmentioning

confidence: 99%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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“…They all lie in the region of the diagram defined by P spin /P orb < 0.01, but with a large range of orbital periods. They include the very long outburst interval SU UMa star, WZ Sge (Patterson et al 1998) with a proposed spin period of 28 s, the propeller system AE Aqr (Choi, Dotani & Agrawal 1999) with a 33 s spin period, the 'DQ Her systems' V533 Her (Thorstensen & Taylor 2000) and DQ Her (Zhang et al 1995), and also XY Ari (Hellier, Mukai & Beardmore 1997) and the long orbital period old nova GK Per (Morales-Rueda, Still & Roche 1996).…”

Section: Rapid Rotatorsmentioning

confidence: 99%

The Spin Periods of Magnetic Cataclysmic Variables

Norton

Somerscales

Wynn

2004

International Astronomical Union Colloquium

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Abstract. We have used a model of magnetic accretion to investigate the rotational equilibria of magnetic cataclysmic variables (MCVs). This has enabled us to derive a set of equilibrium spin periods as a function of orbital period and magnetic moment which we use to estimate the magnetic moments of all known intermediate polars. We further show how these equilibrium spin periods relate to the polar synchronisation condition and use these results to calculate the theoretical histogram describing the distribution of magnetic CVs as a function of P spin /P orb . We demonstrate that this is in remarkable agreement with the observed distribution assuming that the number of systems as a function of white dwarf magnetic moment is distributed according to N (µ 1 )dµ 1 ∝ µ −2 1 dµ 1 . The sample of MCVsAs shown in Figure 1, the MCVs occupy a wide range of parameter space in the spin period (P spin ) versus orbital period (P orb ) plane. This indicates that accretion occurs by a variety of different types of magnetically controlled flow. However, certain regions of the diagram are sparsely populated. In order to understand this distribution we use a model of magnetic accretion to investigate the rotational equilibria of these systems. First we discuss the systems included in Figure 1 and their characteristics. Synchronous polarsWe include 67 synchronous polars ranging from CV Hyi with a period of 77.8 min to V1309 Ori with a period of 7.98 h. Magnetic field strength estimates exist for 52 of these, spanning the range µ 1 ∼ 3 × 10 33 − 10 35 G cm 3 . It is apparent that a true period gap no longer exists for polars, however we note that there are 22 synchronous systems with P spin = P orb > 2.5 h and a further 45 systems with P spin = P orb < 2.5 h. 216

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“…5, see also [17] for CCD V band light curve between A recent brightening of X Ser in Fig. 6b has the decaying rate which correspond to Bailey relation [1] of dwarf-nova outburst in a CV with an exceptionally long orbital period (for P orb = 1.498 d [43]). Also the rising branch of this brightening speaks in favor of a dwarf nova outburst.…”

Section: Serpentismentioning

confidence: 53%

Cataclysmic Variables - a Reach Laboratory for Accretion Processes

Šimon¹

2017

Proceedings of Frontier Research in Astrophysics – II — PoS(FRAPWS2016)

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We show that cataclysmic variables (CVs) are important laboratories for investigation of accretion processes. It is important that a CV binary works as a system strongly variable with time. The character of the long-term activity (and operation of the emission processes) largely depend on the mass inflow into the lobe of the WD, and on the strength of the magnetic field of this WD. Strong structural changes of the emitting regions with time often accompany the transitions between the states of activity. Cycles of this activity (often on timescale of months to years) are common. Episodic events are the common properties of this activity which often consists of the discrete levels of intensity and/or discrete phenomena (e.g. outbursts, low state episodes). We also show that classical nova explosion has the large consequences for the type of activity (and even its change) after returning to quiescence in some CVs. Investigation of interplay of various emitting regions (and emission processes) in various states of activity is very important.

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Spectroscopy and orbital periods of the old novae V533 Herculis, V446 Herculis and X Serpentis

Cited by 52 publications

References 29 publications

SALT observations of southern post-novae

SALT observations of southern post-novae

The Spin Periods of Magnetic Cataclysmic Variables

Cataclysmic Variables - a Reach Laboratory for Accretion Processes

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