INFRARED PHOTOMETRY AND SPECTROSCOPY OF VY Aqr AND EI Psc: TWO SHORT-PERIOD CATACLYSMIC VARIABLES WITH CURIOUS SECONDARY STARS

Harrison, T. E.; Bornak, Jillian; Howell, Steve B.; Mason, E.; Szkody, Paula; McGurk, Rosalie

doi:10.1088/0004-6256/137/4/4061

Cited by 14 publications

(15 citation statements)

References 26 publications

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“…Two objects fall near the main sequence relationship: EI Psc, and RZ Leo. As discussed in Harrison et al (2009) EI Psc (P orb = 1.07 hr) acts just like a main sequence K5 dwarf in the infrared, and apparently suffers from very little accretion disk contamination. The other object, RZ Leo, has such uncertain photometry (∼ ±0.2 mags, see Table 2) that its position in the diagram is very poorly constrained and does not allow for any conclusions.…”

Section: Discussionmentioning

confidence: 91%

“…In Figure 6 we have plotted our new spectral type estimates on the empirical donor sequence (Knigge 2006). We have also added the results from Harrison et al (2009) for EI Psc and VY Aqr to this diagram for completeness. Overall we find that our estimates fit well with Knigge's empirical fit.…”

Section: Discussionmentioning

confidence: 99%

“…Howell et al (2010) presented the K-band spectrum of RZ Leo, which showed no evidence of a C deficit manifested as weakened or absent CO features. Harrison et al (2009) obtained moderate resolution observations VY Aqr and EI Psc, finding evidence for strong deficits of C in both systems. Howell et al (2004) presented observations of WZ Sge, showing this object to have both CO and H 2 emission from its accretion disk, the only such detection so far.…”

Section: Introductionmentioning

confidence: 90%

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Infrared Spectroscopic Observations of the Secondary Stars of Short-Period Sub-Gap Cataclysmic Variables

Hamilton

Harrison

Tappert

et al. 2011

ApJ

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We present K-band spectroscopy of short period, "sub-gap" cataclysmic variable (CV) systems obtained using ISAAC on the VLT. We show the infrared spectra (IR) for nine systems below the 2-3 hour period gap: V2051 Oph, V436Cen, EX Hya, VW Hyi, Z Cha, WX Hyi, V893 Sco, RZ Leo, and TY PsA. We are able to clearly detect the secondary star in all but WX Hyi, V893 Sco, and TY PsA. We present the first direct detection of the secondary stars of V2051 Oph, V436 Cen, and determine new spectral classifications for EX Hya, VW Hyi, Z Cha, and RZ Leo. We find that the CO band strengths of all but Z Cha appear normal for their spectral types, in contrast to their longer period cousins above the period gap. This brings the total number of CVs and pre-CVs with moderate resolution (R 1500) IR spectroscopy to sixty-one systems: nineteen pre-CVs, thirty-one non-magnetic systems, and eleven magnetic or partially magnetic systems. We discuss the trends seen in the IR abundance patterns thus far, and highlight a potential link between anomalous abundances seen in the IR with the C IV/N V anomaly seen in the ultraviolet. We present a compilation of all systems with sufficient resolution IR observations to assess the CO band strengths, and, by proxy, obtain an estimate on the C abundance on the secondary star.

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Section: Discussionmentioning

confidence: 91%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 90%

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Infrared Spectroscopic Observations of the Secondary Stars of Short-Period Sub-Gap Cataclysmic Variables

Hamilton

Harrison

Tappert

et al. 2011

ApJ

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“…Assuming a similar inclination, we find from binary light curve modeling (cf. Harrison et al 2009) that even the shortest period companions would produce less V band variation from reflection effects than we see in Figure 2. PNNi are too bright, washing out any variations due to reflection from companions.…”

Section: Limits On Stellar Companionsmentioning

confidence: 57%

ASTROMETRY WITH THEHUBBLE SPACE TELESCOPE: TRIGONOMETRIC PARALLAXES OF PLANETARY NEBULA NUCLEI NGC 6853, NGC 7293, ABELL 31, AND DeHt 5

Benedict¹,

McArthur²,

Napiwotzki

et al. 2009

The Astronomical Journal

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We present absolute parallaxes and relative proper motions for the central stars of the planetary nebulae NGC 6853 (The Dumbbell), NGC 7293 (The Helix), Abell 31, and DeHt 5. This paper details our reduction and analysis using DeHt 5 as an example. We obtain these planetary nebula nuclei (PNNi) parallaxes with astrometric data from Fine Guidance Sensors FGS 1R and FGS 3, white-light interferometers on the Hubble Space Telescope (HST). Proper motions, spectral classifications and VJHKT 2 M and DDO51 photometry of the stars comprising the astrometric reference frames provide spectrophotometric estimates of reference star absolute parallaxes. Introducing these into our model as observations with error, we determine absolute parallaxes for each PNN. Weighted averaging with previous independent parallax measurements yields an average parallax precision, σ π /π = 5%. Derived distances are: d N GC 6853 = 405 +28 −25 pc, d N GC 7293 = 216 +14 −12 pc, d Abell 31 = 621 +91 −70 pc, and d DeHt 5 = 345 +19 −17 pc. These PNNi distances are all smaller than previously derived from spectroscopic analyses of the central stars. To obtain absolute magnitudes from these distances requires estimates of interstellar extinction. We average extinction measurements culled -2from the literature, from reddening based on PNNi intrinsic colors derived from model SEDs, and an assumption that each PNN experiences the same rate of extinction as a function of distance as do the reference stars nearest (in angular separation) to each central star. We also apply Lutz-Kelker bias corrections. The absolute magnitudes and effective temperatures permit estimates of PNNi radii, through both the Stefan-Boltzmann relation and Eddington fluxes. Comparing absolute magnitudes with post-AGB models provides mass estimates. Masses cluster around 0.57 M ⊙ , close to the peak of the white dwarf mass distribution. Adding a few more PNNi with well-determined distances and masses, we compare all the PNNi with cooler white dwarfs of similar mass, and confirm, as expected, that PNNi have larger radii than white dwarfs that have reached their final cooling tracks.Subject headings: astrometry -interferometry -planetary nebulae -stars: distances -stars: white dwarf -stars: masses Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. This research has made use of the SIMBAD database and Aladin, both developed at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED) which is operated by JPL, California Institute of Technology, under contract with the NASA; and NASA's Astrophysics Data System Abstract Service. We thank an anonymous referee for a careful reading and suggestions that improved the presentation.

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“…Recently some new objects (EI Psc, OZ Ser, CSS100531) were discovered with very hot donor stars (∼K4V spectral type) [13,14,15]. They probably form an additional subclass of CVs in the discussed period range.…”

Section: Geometry Of Short Orbital Period Cvs Primaries and Secondariesmentioning

confidence: 99%

Short Orbital Period Cataclysmic Variables

Zharikov¹

2017

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects - III — PoS(Golden2015)

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Cataclysmic Variables (CVs) are semi-detached binary systems consisting red/brown dwarfs filling its corresponding Roche lobe and loosing matter onto white dwarf (WD) companions. Classification of CVs is based on behavior of outbursts. In this report, we review properties of Short Orbital Period Cataclysmic Variables (77 min < P orb < 120 min). In mentioned orbital period range three subclasses of CVs were distinguished: SU UMa-, ER UMa-and WZ Sge-type objects. WZ Sge-type objects more probably includes also systems evolved past of the period minimum. The last are formed so-called bounce-backs or post-period minimum systems. Main characteristics of WDs, donor stars and accretion disks in the Short Orbital Period Cataclysmic Variables are discussed.

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INFRARED PHOTOMETRY AND SPECTROSCOPY OF VY Aqr AND EI Psc: TWO SHORT-PERIOD CATACLYSMIC VARIABLES WITH CURIOUS SECONDARY STARS

Cited by 14 publications

References 26 publications

Infrared Spectroscopic Observations of the Secondary Stars of Short-Period Sub-Gap Cataclysmic Variables

Infrared Spectroscopic Observations of the Secondary Stars of Short-Period Sub-Gap Cataclysmic Variables

ASTROMETRY WITH THEHUBBLE SPACE TELESCOPE: TRIGONOMETRIC PARALLAXES OF PLANETARY NEBULA NUCLEI NGC 6853, NGC 7293, ABELL 31, AND DeHt 5

Short Orbital Period Cataclysmic Variables

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