A New, Bright, Short-Period, Emission Line Binary in Ophiuchus

Stark, M. A.; Wade, Richard A.; Thorstensen, J. R.; Peters, C. S.; Smith, Horace A.; Miller, Robert D.; Green, E. M.

doi:10.1088/0004-6256/135/3/991

Cited by 4 publications

(21 citation statements)

References 18 publications

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“…It entered the observing program only as a backup target. However, as it turns out, the present additional observations nicely complement those of Stark et al (2008).…”

Section: Introductionsupporting

confidence: 87%

“…2 of Stark et al (2008) and which is quite typical for CVs with accretion disks in the bright state: Balmer emission components decreasing in strength from Hα to Hβ are superposed upon broad absorption troughs which are stronger for the higher Balmer lines. It appears that the centre of the Hα absorption is somewhat shifted to the blue with respect to the emission component.…”

Section: Spectra Of Ls IV -08mentioning

confidence: 90%

“…The characteristics of the system suggested a reclassification as a nova-like variable of the UX UMa subtype. Stark et al (2008) also present some time resolved photometry which reveals low scale (a few hundredths of a magnitude) apparently stochastic variations …”

Section: Ls IV -08mentioning

confidence: 92%

“…LS IV -08 o 3 was originally classified as an OB star (Nassau & Stephensen, 1963). Stark et al (2008) narrate more of the history of our knowledge about this object. They performed a detailed spectroscopic study and found that LS IV -08 o 3 is a binary with a period of 0.1952894 days.…”

Section: Ls IV -08mentioning

confidence: 99%

“…On the other hand, LS IV -08 o 3 was quite thoroughly characterized by Stark et al (2008). It entered the observing program only as a backup target.…”

Section: Introductionmentioning

confidence: 99%

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Time resolved spectroscopy and photometry of three little known bright cataclysmic variables: LS IV −08° 3, HQ Monocerotis and ST Chamaeleontis

Bruch

Diaz

2017

New Astronomy

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As part of a project to better characterize comparatively bright but so far little studied cataclysmic variables in the southern hemisphere, we have obtained spectroscopic and photometric data of the nova-like variables LS IV -08 o 3 and HQ Mon, and of the Z Cam type dwarf nova ST Cha. The spectra of all systems are as expected for their respective types. We derive improved orbital ephemeris of LS IV -08 o 3 and map its accretion disk in the light of the Hα emission using Doppler tomography. We find that the emission has a two component origin, arising in the outer parts of the accretion disk and possibly on the illuminated face of the secondary star. The light curve of LS IV -08 o 3 exhibits a low level of flickering and indications for a modulation on the orbital period. Spectroscopy of HQ Mon suggests an orbital period of ≈ 5 h .15 which is incompatible with previous (uncertain) estimates. The light curves show the typical low scale flickering of UX UMa type nova-like systems, superposed upon variations on longer time scales. During one night a modulation with a period of ≈ 41 m is observed, visible for at least 4 hours. However, it does not repeat itself in other nights. A spectroscopic orbital period of ≈ 5 h .5 is derived for ST Cha. A previously suspected period of 6 h .8 (or alternatively 9 h .6), based on historical photographic photometry is incompatible with the spectroscopic period. Moreover, we show that our new as well as previous photometry does not contain evidence for the quoted photometric period.

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“…It entered the observing program only as a backup target. However, as it turns out, the present additional observations nicely complement those of Stark et al (2008).…”

Section: Introductionsupporting

confidence: 87%

Section: Spectra Of Ls IV -08mentioning

confidence: 90%

Section: Ls IV -08mentioning

confidence: 92%

Section: Ls IV -08mentioning

confidence: 99%

“…On the other hand, LS IV -08 o 3 was quite thoroughly characterized by Stark et al (2008). It entered the observing program only as a backup target.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Time resolved spectroscopy and photometry of three little known bright cataclysmic variables: LS IV −08° 3, HQ Monocerotis and ST Chamaeleontis

Bruch

Diaz

2017

New Astronomy

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A MeerKAT survey of nearby nova-like cataclysmic variables

Hewitt

Pretorius

Woudt

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ${\gtrsim}2.2\times 10^{18}\,$ erg s−1 Hz−1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the $L_X\propto L_R^{\sim 0.7}$ power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9–1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.

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SDSS unveils a population of intrinsically faint cataclysmic variables at the minimum orbital period

Gänsicke

Dillon

Southworth

et al. 2009

Monthly Notices of the Royal Astronomical Society

265

338

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We discuss the properties of 137 cataclysmic variables (CVs) which are included in the Sloan Digital Sky Survey (SDSS) spectroscopic data base, and for which accurate orbital periods have been measured. 92 of these systems are new discoveries from SDSS and were followed‐up in more detail over the past few years. 45 systems were previously identified as CVs because of the detection of optical outbursts and/or X‐ray emission, and subsequently re‐identified from the SDSS spectroscopy. The period distribution of the SDSS CVs differs dramatically from that of all the previously known CVs, in particular it contains a significant accumulation of systems in the orbital period range 80–86 min. We identify this feature as the elusive ‘period minimum spike’ predicted by CV population models, which resolves a long‐standing discrepancy between compact binary evolution theory and observations. We show that this spike is almost entirely due to the large number of CVs with very low accretion activity identified by SDSS. The optical spectra of these systems are dominated by emission from the white dwarf photosphere, and display little or no spectroscopic signature from the donor stars, suggesting very low mass companion stars. We determine the average absolute magnitude of these low‐luminosity CVs at the period minimum to be 〈Mg〉= 11.6 ± 0.7. Comparison of the SDSS CV sample to the CVs found in the Hamburg Quasar Survey and the Palomar Green Survey suggests that the depth of SDSS is the key ingredient resulting in the discovery of a large number of intrinsically faint short‐period systems.

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A New, Bright, Short-Period, Emission Line Binary in Ophiuchus

Cited by 4 publications

References 18 publications

Time resolved spectroscopy and photometry of three little known bright cataclysmic variables: LS IV −08° 3, HQ Monocerotis and ST Chamaeleontis

Time resolved spectroscopy and photometry of three little known bright cataclysmic variables: LS IV −08° 3, HQ Monocerotis and ST Chamaeleontis

A MeerKAT survey of nearby nova-like cataclysmic variables

SDSS unveils a population of intrinsically faint cataclysmic variables at the minimum orbital period

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