Mr. Clarke to William Bowyer, 18 December 1732

Clarke, Henry Leland; Williams, Harold

doi:10.1093/oseo/instance.00042302

Cited by 2 publications

(2 citation statements)

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“…While most dwarf novae, including RX And itself (cf. Clarke, Bowyer (1984); Kaitchuck et al (1988)) are known to show reduced line strengths above quiescence, RX And in this stage showed relatively strong emission lines. This suggests that the accretion disk had an extra emission source, which can be naturally explained if the heating wave from the inner region had not reached the outer region of the accretion disk and the accumulated matter during the low quiescence was left from being accreted.…”

Section: Brightening From the Minimummentioning

confidence: 96%

Extended Deep Minimum and Subsequent Brightening of RX And in 1996-1997

Katô

Nogami

Masuda

2002

Publications of the Astronomical Society of Japan

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We discovered that RX And, one of prototypical Z Camtype dwarf novae, underwent a deep, extended faint state in 1996-1997. Time-resolved photometry at the bottom of the fading revealed the presence of strong flickering, and the absence of detectable orbital modulation. This finding indicates that the mass-transfer remained even at the deepest minimum of the fading, contrary to what was observed in a deep minimum of a VY Scl-type star, MV Lyr. RX And subsequently underwent a brightening (outburst) during its recovery stage. The photometric and spectroscopic characteristics of the brightening significantly differed from those of ordinary outbursts of RX And, and are considered to resemble an inside-out type outburst of a long-period dwarf nova. An examination of historical visual observations revealed the possible presence of ∼10-yr periodicity, which is close to what has been proposed for MV Lyr. The common observed features between RX And and VY Scl-type stars may suggest a common underlying mechanism for producing temporary deep fadings. The departure from the disk instability model, as observed in VY Scl-type stars, was not apparent in the present fading of RX And. In conjunction with the recently published Hubble Space Telescope observation during the same fading, we can conclude that the phenomenological difference from the VY Scl-type fading is understood as a smaller effect of irradiation on the accretion disk in RX And.

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Section: Brightening From the Minimummentioning

confidence: 96%

Extended Deep Minimum and Subsequent Brightening of RX And in 1996-1997

Katô

Nogami

Masuda

2002

Publications of the Astronomical Society of Japan

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“…The inversion of Balmer emission lines to absorption is common for dwarf novae in outburst (e.g. Clarke & Bowyer 1984;Neustroev et al 2017). This contrasts to what was observed during the superoutburst of the bounce-back candidate V455 And (Tovmassian et al 2011).…”

Section: Outburstmentioning

confidence: 99%

From outburst to quiescence: spectroscopic evolution of V1838 Aql imbedded in a bow-shock nebula

Santisteban

Echevarría

Zharikov

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We analyse new optical spectroscopic, direct-image and X-ray observations of the recently discovered a high proper motion cataclysmic variable V1838 Aql. The data were obtained during its 2013 superoutburst and its subsequent quiescent state. An extended emission around the source was observed up to 30 days after the peak of the superoutburst, interpreted it as a bow-shock formed by a quasi-continuous outflow from the source in quiescence. The head of the bow-shock is coincident with the highproper motion vector of the source (v ⊥ = 123 ± 5 km s −1 ) at a distance of d = 202 ± 7 pc. The object was detected as a weak X-ray source (0.015 ± 0.002 counts s −1 ) in the plateau of the superoutburst, and its flux lowered by two times in quiescence (0.007±0.002 counts s −1 ). Spectroscopic observations in quiescence we confirmed the orbital period value P orb = 0.0545 ± 0.0026 days, consistent with early-superhump estimates, and the following orbital parameters: γ = −21 ± 3 km s −1 and K 1 = 53 ± 3 km s −1 . The white dwarf is revealed as the system approaches quiescence, which enables us to infer the effective temperature of the primary T e f f = 11, 600 ± 400K. The donor temperature is estimated 2200K and suggestive of a system approaching the period minimum. Doppler maps in quiescence show the presence of the hot spot in HeI line at the expected accretion disc-stream shock position and an unusual structure of the accretion disc in Hα.

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Mr. Clarke to William Bowyer, 18 December 1732

Cited by 2 publications

References 0 publications

Extended Deep Minimum and Subsequent Brightening of RX And in 1996-1997

Extended Deep Minimum and Subsequent Brightening of RX And in 1996-1997

From outburst to quiescence: spectroscopic evolution of V1838 Aql imbedded in a bow-shock nebula

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