The new pre-cataclysmic binary PG 2200+085

Shimansky, V. V.; Сахибуллин, Н. А.; Bikmaev, I.; Ritter, H. G.; Suleimanov, V.; Borisov, N. V.; Galeev, A.

doi:10.1051/0004-6361:20065146

Cited by 24 publications

(19 citation statements)

References 64 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Among ∼40 previously known PCEBs listed in Schreiber & Gänsicke (2003), and Shimansky et al (2006), only 8 systems display a reflection effect comparable to that of HS 1857+5144 (Table 3). All those systems contain extremely hot white dwarfs or subdwarfs, and all are very young PCEBs that may serve as observational probes into our understanding of common envelope evolution.…”

Section: Discussionmentioning

confidence: 85%

HS 1857+5144: a hot and young pre-cataclysmic variable

Aungwerojwit

Gänsicke

Rodríguez‐Gil

et al. 2007

A&A

View full text Add to dashboard Cite

Aims. We report the discovery of a new white dwarf/M dwarf binary, HS 1857+5144, identified in the Hamburg Quasar Survey (HQS). Methods. Time-resolved optical spectroscopy and photometry were carried out to determine the properties of this new cataclysmic variable progenitor (pre-CV). Results. The light curves of HS 1857+5144 display a sinusoidal variation with a period of P orb = 383.52 min and peak-to-peak amplitudes of 0.7 mag and 1.1 mag in the B-band and R-band, respectively. The large amplitude of the brightness variation results from a reflection effect on the heated inner hemisphere of the companion star, suggesting a very high temperature of the white dwarf. Our radial velocity study confirms the photometric period as the orbital period of the system. A model atmosphere fit to the spectrum of the white dwarf obtained at minimum light provides limits to its mass and temperature of M wd 0.6−1.0 M and T wd 70 000−100 000 K, respectively. The detection of He II λ4686 absorption classifies the primary star of HS 1857+5144 as a DAO white dwarf. Combining the results from our spectroscopy and photometry, we estimate the mass of the companion star and the binary inclination to be M sec 0.15−0.30 M and i 45• −55 • , respectively. Conclusions. We classify HS 1857+5144 as one of the youngest pre-CV known to date. The cooling age of the white dwarf suggests that the present system has just emerged from a common envelope phase ∼10 5 yr ago. HS 1857+5144 will start mass transfer within or below the 2-3 h period gap.

show abstract

Section: Discussionmentioning

confidence: 85%

HS 1857+5144: a hot and young pre-cataclysmic variable

Aungwerojwit

Gänsicke

Rodríguez‐Gil

et al. 2007

A&A

View full text Add to dashboard Cite

show abstract

“…To explore the parameter space we enlarged the sample by taking the PCEB lists of Morales-Rueda et al (2005) and Shimansky et al (2006), examined the published data on these systems, and included HS 1857+5144 (Aungwerojwit et al 2007). Since our main interest concerns potential precataclysmic variables such as LTT 560, we limited the sample to PCEBs with P orb < 1 d that contain a white dwarf as primary component.…”

Section: Discussionmentioning

confidence: 99%

Multiple emission line components in detached post-common-envelope binaries

Tappert

Gänsicke

Rebassa‐Mansergas

et al. 2011

A&A

View full text Add to dashboard Cite

Motivated by the recent discovery of an Hα emission line component originating close to the white dwarf primary in the post-commonenvelope binary (PCEB) LTT 560, we have undertaken a spectroscopic snapshot survey on 11 short-period (P orb < 6 h) PCEBs using FORS2. We have found multi-component Hα emission line profiles in six of our targets, indicating that multiple Hα emission sites are rather common in short-period PCEBs. The underlying physical mechanisms, however, can be fundamentally different. In our sample we find one system where the extracted radial velocities of two identified components indicate that both originate in the late-type secondary star, where one is caused by irradiation from the hot white dwarf primary and the other by stellar activity. Another object presents two components that are located on opposite sides of the centre-of-mass, suggesting a case similar to LTT 560, i.e. that accretion of stellar wind from the secondary star produces Hα emission on, or close to, the white dwarf.

show abstract

“…Liebert et al (2005) noted the absence of non-accreting magnetic white dwarfs (MWDs) among the more than 1200 WDMS binaries compiled by Silvestri et al (2007) and various other samples (Marsh 2000;Ritter & Kolb 2003;Schreiber & Gänsicke 2003;Morales-Rueda et al 2005;Shimansky et al 2006). MWDs are clearly underrepresented in current WDMS samples compared to the ∼10% fraction in the field (Liebert et al 2003).…”

Section: Discussionmentioning

confidence: 99%

Post common envelope binaries from the SDSS

Schwope¹,

Gómez‐Morán²,

Schreiber

et al. 2009

A&A

View full text Add to dashboard Cite

We report the discovery of the ninth pre-polar consisting of a late-type ZAMS secondary and a magnetic white dwarf. The white dwarf accretes at an extreme low rate,Ṁ ∼ 10 −14 M yr −1 , from the wind of the companion donor star. The source was found in our systematic search for WD/MS binaries within SDSS/SEGUE. Based on seven Sloan spectra we estimate a binary period of ∼200, 230, or 270 min. The UV to IR spectral energy distribution was decomposed into a dM3-dM4 ZAMS secondary and a cool white dwarf, ∼9000 K, which consistently imply a distance between 360 and 420 pc. The optical spectrum displays one pronounced cyclotron hump, likely originating from a low-temperature plasma, ∼1 keV, in a field of 108 MG. We comment on the evolutionary link between polars and pre-polars.

show abstract

The new pre-cataclysmic binary PG 2200+085

Cited by 24 publications

References 64 publications

HS 1857+5144: a hot and young pre-cataclysmic variable

HS 1857+5144: a hot and young pre-cataclysmic variable

Multiple emission line components in detached post-common-envelope binaries

Post common envelope binaries from the SDSS

Contact Info

Product

Resources

About