Wozu berufliche Qualifizierung?

Haefner, Klaus

doi:10.1007/978-3-0348-5374-3_6

Cited by 8 publications

(18 citation statements)

References 1 publication

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“…An extended shell with a complex shape around RR Pic has been known and has been well documented for long time (Williams & Gallagher 1979;Duerbeck & Seitter 1979;Gill & O'Brien 1998;Downes & Duerbeck 2000). Some authors (Haefner & Metz 1982;Warner 1986) have suggested that the nova is an eclipsing binary with P = 3.…”

Section: Rr Picmentioning

confidence: 96%

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: Rr Picmentioning

confidence: 96%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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“…For RR Pic, Haefner & Metz (1982) had presented a model with a ratio q = 0.42, larger than the critical value expected to present superhumps. While their adopted WD mass of 0.95 M ⊙ is in good agreement with a recent model by Sion et al (2017) based on far UV spectroscopy (∼ 1 M ⊙ ) the mass of the secondary seems to be smaller, according to a systematic investigation the properties of the secondary stars in CVs by Smith & Dhillon (1998).…”

Section: Rr Pic In Context With Other Superhumpersmentioning

confidence: 94%

“…(iii) Light curves in five nights observed in January 1980 by Haefner & Metz (1982) in the V band. In all of them at least one complete orbital cycle was observed.…”

Section: Compilation Of Historical Light Curves and New Observationsmentioning

confidence: 99%

“…The light curves of Haefner & Metz (1982) and Kubiak (1984) were only available as figures. Therefore, we digitised them from the respective publications, using the Dexter 2 service from the website of the German Astrophysical Virtual Observatory (GAVO).…”

Section: Compilation Of Historical Light Curves and New Observationsmentioning

confidence: 99%

“…Time-series spectroscopy and Doppler mapping found evidence for two emission sources, the hotspot and a source opposite. (Haefner & Metz 1982;Schmidtobreick et al 2003;Ribeiro & Diaz 2006). In a recent work Vogt et al (2017) derived a more precise orbital ephemeris from all available photometric humps observed in the past five decades.…”

Section: Introductionmentioning

confidence: 99%

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Photometric long-term variations and superhump occurrence in the Classical Nova RR Pictoris

Fuentes-Morales¹,

Vogt²,

Tappert³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present an analysis of all available time-resolved photometry from the literature and new light curves obtained in 2013-2014 for the old nova RR Pictoris. The well-known hump light curve phased with the orbital period reveals significant variations over the last 42 years in shape, amplitude and other details which apparently are caused by long-term variations in the disc structure. In addition we found evidence for the presence of superhumps in 2007, with the same period (∼9% longer than the orbital period), as reported earlier by other authors from observations in 2005. Possibly, superhumps arise quickly in RR Pic, but are sporadic events, because in all the other observing runs analysed no significant superhump signal was detected. We also determined an actual version of the Stolz-Schoembs relation between superhump period and orbital period, analysing separately dwarf novae, classical novae and nova-like stars, and conclude that this relation is of general validity for all superhumpers among the cataclysmic variables (CVs), in spite of small but significant differences among the sub-types mentioned above. We emphasize the importance of such a study in context with the still open question of the interrelation between the different sub-classes of CVs, crucial for our understanding of the long-term CV evolution.

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The emission distribution in RR Pictoris

Schmidtobreick

Tappert

Saviane

2003

Monthly Notices of the Royal Astronomical Society

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We present time-resolved optical spectroscopy of the old nova RR Pic. Two emission lines (Hα and He I) are present in the observed part of the spectrum and both show strong variability. Hα has been used for Doppler tomography in order to map the emission distribution in this system for the first time. The resulting map shows the emission from the disc as well as two additional emission sources on the leading and trailing sides of the disc. Furthermore, we find evidence for the presence of either a disc overflow or an asymmetric outflow from the binary with velocities up to ±1200 km s −1 . The origin of the outflow would be the emission source on the leading side of the accretion disc.

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Wozu berufliche Qualifizierung?

Cited by 8 publications

References 1 publication

SALT observations of southern post-novae

SALT observations of southern post-novae

Photometric long-term variations and superhump occurrence in the Classical Nova RR Pictoris

The emission distribution in RR Pictoris

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