The ultraviolet pulsations of the cataclysmic variable AE Aquarii as observed with the Hubble Space Telescope

Eracleous, Michael; Horne, K.; Robinson, E. L.; Zhang, Er Ho; Marsh, T. R.; Wood, Janet H.

doi:10.1086/174647

Cited by 81 publications

(133 citation statements)

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“…Bitner et al (2007) provided estimates for the masses of the secondary star and the WD in SS Cygni (M WD = 0.81 M , M s = 0.55 M ) and presented a discussion on the unusual evolutionary characteristics of the secondary and Sion et al (2010) presented an extended analysis of its carbon-poor UV spectrum. Similar behavior has been observed for the CV AE Aqr (Jameson et al 1980;Eracleous et al 1994). Harrison et al (2005) presented more cases of CVs with weak CO absorption lines in their spectra, implying low C abundance, and suggested that material that has been processed through the CNO cycle is finding its way into the photospheres of secondary stars.…”

Section: Introductionsupporting

confidence: 77%

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

Chatzopoulos¹,

Robinson²,

Wheeler³

2012

ApJ

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Many population synthesis and stellar evolution studies have addressed the evolution of close binary systems in which the primary is a compact remnant and the secondary is filling its Roche lobe, thus triggering mass transfer. Although tidal locking is expected in such systems, most studies have neglected the rotationally induced mixing that may occur. Here we study the possible effects of mixing in mass-losing stars for a range of secondary star masses and metallicities. We find that tidal locking can induce rotational mixing prior to contact and thus affect the evolution of the secondary star if the effects of the Spruit-Tayler dynamo are included both for angular momentum and chemical transport. Once contact is made, the effect of mass transfer tends to be more rapid than the evolutionary timescale, so the effects of mixing are no longer directly important, but the mass-transfer strips matter to inner layers that may have been affected by the mixing. These effects are enhanced for secondaries of 1-1.2 M and for lower metallicities. We discuss the possible implications for the paucity of carbon in the secondaries of the cataclysmic variable SS Cyg and the black hole candidate XTE J1118+480 and for the progenitor evolution of Type Ia supernovae. We also address the issue of the origin of blue straggler stars in globular and open clusters. We find that for models that include rotation consistent with that observed for some blue straggler stars, evolution is chemically homogeneous. This leads to tracks in the H-R diagram that are brighter and bluer than the non-rotating main-sequence turn-off point. Rotational mixing could thus be one of the factors that contribute to the formation of blue stragglers.

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Section: Introductionsupporting

confidence: 77%

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

Chatzopoulos¹,

Robinson²,

Wheeler³

2012

ApJ

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“…The oscillation has two unequal peaks per spin cycle, consistent with broad hotspots on opposite sides of the white dwarf ~ 15° above and below the equator (Eracleous et al 1994). These oscillations are strongest in the ultraviolet, where their spectra show a blue continuum with broad Ly a absorption consistent with a white dwarf (log # ss 8) atmosphere with T~3 x 10 4 K (Eracleous et al 1994). The simplest interpretation is accretion heating near the poles of a magnetic dipole field tipped almost perpendicular to the rotation axis.…”

Section: Introductionmentioning

confidence: 76%

Section: Introductionmentioning

confidence: 98%

“…Coherent oscillations in optical (Patterson 1979), ultraviolet (Eracleous et al 1994), and X-ray (Patterson et al 1980) lightcurves reveal the white dwarf's 33s spin period. The oscillation has two unequal peaks per spin cycle, consistent with broad hotspots on opposite sides of the white dwarf ~ 15° above and below the equator (Eracleous et al 1994). These oscillations are strongest in the ultraviolet, where their spectra show a blue continuum with broad Ly a absorption consistent with a white dwarf (log # ss 8) atmosphere with T~3 x 10 4 K (Eracleous et al 1994).…”

Section: Introductionmentioning

confidence: 98%

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Fireballs, Flares and Flickering

Pearson

Horne

Skidmore

2004

International Astronomical Union Colloquium

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Abstract. We review our understanding of the prototype "Propeller" system AE Aqr and we examine its flaring behaviour in detail. The flares are thought to arise from collisions between high density regions in the material expelled from the system after interaction with the rapidly rotating magnetosphere of the white dwarf. We show calculations of the time-dependent emergent optical spectra from the resulting hot, expanding ball of gas and derive values for the mass, lengthscale and temperature of the material involved. We see that the fits suggest that the secondary star in this system has reduced metal abundances and that, counterintuitively, the evolution of the fireballs is best modelled as isothermal.

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“…AE Aqr, already mentioned above, has an unknown T e f f because the dominant measurable UV flux comes from spots with T ∼ 26 000 K produced by heating by the accretion columns (Eracleous et al 1994). If the general non-heated surface temperature of the primary could be measured more accurately than the currently estimated 10 000 -16 000 K this would provide a measure of how long ago the highṀ phase (characteristic of the large P orb of AE Aqr) was interrupted, probably by a nova eruption.…”

Section: Magnetic Novaementioning

confidence: 98%

General Properties of Quiescent Novae

Warner

2002

AIP Conference Proceedings

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Abstract.The observed properties of novae before and after eruption are discussed. The distribution of orbital periods of novae shows a concentration near 3.2 h, which resembles that of magnetic cataclysmic variables, and there is some evidence that many of the novae themselves are magnetic near that orbital period. Desynchronisation of polars by nova eruptions can lead to an estimate (∼ 2 × 10 3 y) for the time between eruptions for the strongly magnetic systems; this is much shorter than that found from other methods. The similarity of pre-and post-nova luminosities, at high rates of mass transfer, is ascribed to irradiation of the secondary producing a self-sustained higḣ M state. This slows cooling of the white dwarf after eruption, delays the onset of full scale dwarf nova outbursts in most systems, and delays any descent into a hibernation state of low rate of mass transfer.

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The ultraviolet pulsations of the cataclysmic variable AE Aquarii as observed with the Hubble Space Telescope

Cited by 81 publications

References 0 publications

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

Effects of Rotationally Induced Mixing in Compact Binary Systems With Low-Mass Secondaries and in Single Solar-Type Stars

Fireballs, Flares and Flickering

General Properties of Quiescent Novae

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