The magnetic SW Sextantis star RX J1643.7+3402

Rodríguez‐Gil, P.; Martínez‐País, I. G.; Rodríguez, J. de la Cruz

doi:10.1111/j.1365-2966.2009.14585.x

Cited by 16 publications

(15 citation statements)

References 23 publications

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“…However, if there is outflow, then it will probably introduce a necessary non-uniformity to the disk edge. The flaring of the emission lines has been interpreted as evidence of magnetic accretion (Rodríguez-Gil et al 2001;Rodríguez-Gil & Martínez-Pais 2002;Rodríguez-Gil et al 2009). This claim is supported by evidence of the periodic nature of flaring, and in some cases, a more substantial indication is the detection Figure 6.…”

Section: Discussionmentioning

confidence: 99%

On the Sw Sex-Type Eclipsing Cataclysmic Variable Sdss0756+0858

Tovmassian

Hernández

González–Buitrago

et al. 2014

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We conducted a spectroscopic and photometric study of SDSS J075653.11+085831. X-ray observations were also attempted. We determined the orbital period of this binary system to be 3.29 hr. It is a deep eclipsing system, whose spectra show mostly single-peaked, Balmer emission lines and a rather intense He ii line. There is also the presence of faint (often double-peaked) He i emission lines as well as several absorption lines, Mg i being the most prominent. All of these features point toward the affiliation of this object with the growing number of SW Sex-type objects. We developed a phenomenological model of an SW Sex system to reproduce the observed photometric and spectral features.

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Section: Discussionmentioning

confidence: 99%

On the Sw Sex-Type Eclipsing Cataclysmic Variable Sdss0756+0858

Tovmassian

Hernández

González–Buitrago

et al. 2014

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“…There is evidence that the WDs in some SW Sex stars are magnetic, based on circular polarimetry observations (Rodríguez‐Gil et al 2001, 2002, 2009). However, the low levels of circular polarization observed suggest WD magnetic field strengths of the order or lower than those observed in the intermediate polar CVs.…”

Section: The Variable Spectrum Of Bb Dor In Quiescencementioning

confidence: 99%

The fight for accretion: discovery of intermittent mass transfer in BB Doradus in the low state

Rodríguez‐Gil¹,

Schmidtobreick²,

Long³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Our long‐term photometric monitoring of southern nova‐like cataclysmic variables with the 1.3‐m Small and Moderate Aperture Research Telescope System (SMARTS) telescope found BB Doradus fading from V∼ 14.3 towards a deep low state at V∼ 19.3 in 2008 April. Here we present time‐resolved optical spectroscopy of BB Dor in this faint state in 2009. The optical spectrum in quiescence is a composite of a hot white dwarf with Teff= 30 000 ± 5000 K and a M3–M4 secondary star with narrow emission lines (mainly of the Balmer series and He i) superposed. We associate these narrow profiles with an origin on the donor star. An analysis of the radial velocity curve of the Hα emission from the donor star allowed the measurement of an orbital period of 0.154 095 ± 0.000 003 d (3.698 28 ± 0.000 07 h), different from all previous estimates. We detected episodic accretion events which veiled the spectra of both stars and radically changed the line profiles within a time‐scale of tens of minutes. This shows that accretion is not completely quenched in the low state. During these accretion episodes the line wings are stronger and their radial velocity curve is delayed by ∼0.2 cycle, similar to that observed in SW Sex and AM Her stars in the high state, with respect to the motion of the white dwarf. Two scenarios are proposed to explain the extra emission: impact of the material on the outer edge of a cold, remnant accretion disc, or the combined action of a moderately magnetic white dwarf (B1≲ 5 MG) and the magnetic activity of the donor star.

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“…Namely, data on the electrical conductivity of plasma of stars with a magnetic field or moving in the magnetic field of the other component in a binary system (see, e.g. Zhang, Wickramasinghe & Ferrario 2009; Rodriguez‐Gil, Martinez‐Pais & Rodriguez 2009; Potter & Tout 2010) could be of significant interest, since they are useful for the study of the thermal evolution of such objects (cooling, nuclear burning of accreted matter) and the investigation of their magnetic fields. For example, Kopecký (1970) and Kopecký & Kotrč (1973) studied electrical conductivity for stars of various spectral types, in order to investigate the magnetohydrodynamic differences in their atmospheres.…”

Section: Introductionmentioning

confidence: 99%

Electrical conductivity of plasmas of DB white dwarf atmospheres

Srećković

Ignjatović

Mihajlov

et al. 2010

Monthly Notices of the Royal Astronomical Society

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The static electrical conductivity of non-ideal, dense, partially ionized helium plasma was calculated over a wide range of plasma parameters: temperatures $1\cdot 10^{4}\textrm{K} \lesssim T \lesssim 1\cdot 10^{5}\textrm{K}$ and mass density $1 \times 10^{-6} \textrm{g}/\textrm{cm}^{3} \lesssim \rho \lesssim 2 \textrm{g}/\textrm{cm}^{3}$. Calculations of electrical conductivity of plasma for the considered range of plasma parameters are of interest for DB white dwarf atmospheres with effective temperatures $1\cdot 10^{4}\textrm{K} \lesssim T_{eff} \lesssim 3\cdot 10^{4}\textrm{K}$. Electrical conductivity of plasma was calculated by using the modified random phase approximation and semiclassical method, adapted for the case of dense, partially ionized plasma. The results were compared with the unique existing experimental data, including the results related to the region of dense plasmas. In spite of low accuracy of the experimental data, the existing agreement with them indicates that results obtained in this paper are correct

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The magnetic SW Sextantis star RX J1643.7+3402

Cited by 16 publications

References 23 publications

On the Sw Sex-Type Eclipsing Cataclysmic Variable Sdss0756+0858

On the Sw Sex-Type Eclipsing Cataclysmic Variable Sdss0756+0858

The fight for accretion: discovery of intermittent mass transfer in BB Doradus in the low state

Electrical conductivity of plasmas of DB white dwarf atmospheres

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