Real Folk

Warner, John O.; Meredith, J. Wayne

doi:10.2307/27516585

Cited by 9 publications

(9 citation statements)

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“…The inclination angle of the binary should be lower than i < 73 • because no eclipses were observed in GK Per (Reinsch 1994). On the other hand, the orbital inclination was estimated, from a correlation between emission-line width and accretion disk inclination, to be ∼ 75 • (Warner 1986), close to the upper limit. If we fix the mass ratio of q = 0.55 at its central value, then we obtain M WD = 1.0 M ⊙ for i = 73 • , M WD = 1.1 M ⊙ for i = 68 • , and M WD = 1.2 M ⊙ for i = 63 • .…”

Section: Discussion On the Results For Gk Permentioning

confidence: 85%

A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

Hachisu

Kato

2007

ApJ

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Optical and infrared light-curves of classical novae are approximately homologous among various white dwarf (WD) masses and chemical compositions when free-free emission from optically thin ejecta is spherical and dominates the continuum flux of novae. Such a homologous template light-curve is called "a universal decline law." Various nova light-curves are approximately reproduced from this universal law by introducing a timescaling factor which stretches or squeezes the template light-curve to match the observation. The timescale of the light curve depends strongly on the WD mass but weakly on the chemical composition, so we are able to roughly estimate the WD mass from the light-curve fitting. We have applied the universal decline law to the old nova GK Persei 1901 and recent novae that outbursted in 2005. The estimated WD mass is 1.15 M ⊙ for GK Per, which is consistent with a central value of the WD mass determined from the orbital velocity variations. The other WD masses of 10 novae in 2005 are also estimated to be 1.05 M ⊙ (V2361 Cyg), 1.15 M ⊙ (V382 Nor), 1.2 M ⊙ (V5115 Sgr), 0.7 M ⊙ (V378 Ser), 0.9 M ⊙ (V5116 Sgr), 1.25 M ⊙ (V1188 Sco), 0.7 M ⊙ (V1047 Cen), 0.95 M ⊙ (V476 Sct), 0.95 M ⊙ (V1663 Aql), and 1.30 M ⊙ (V477 Sct), within a rough accuracy of ±0.1 M ⊙ . Four (V382 Nor, V5115 Sgr, V1188 Sco, and V477 Sct) of ten novae in the year 2005 are probably neon novae on an O-Ne-Mg WD. Each WD mass depends weakly on the chemical composition (especially the hydrogen content X in mass weight), i.e., the obtained WD masses increase by +0.5(X − 0.35) M ⊙ for the six CO novae and by +0.5(X − 0.55) M ⊙ for the four neon novae above. Various nova parameters are discussed in relation to its WD mass.

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Section: Discussion On the Results For Gk Permentioning

confidence: 85%

A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

Hachisu

Kato

2007

ApJ

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“…It was discovered in October of that year, at a time when Harvard objective prism plates were being exposed, whereby it attained the status and alias of HD 321353. The observed maximum was V , 4:5, but it probably reached V , 1:6 (Downes et al 1997), and at minimum it is V , 19, giving it the unusually large eruption amplitude of , 17.5 mag, even for a t 2 ¼ 4 d nova, suggesting a high inclination system (Warner 1986; this conclusion arises from the apparent intrinsic faintness of the nearly edge-on accretion disc which such an object has in quiescence).…”

Section: V630 Saggitariimentioning

confidence: 97%

High-speed photometry of faint cataclysmic variables - I. V359 Cen, XZ Eri, HY Lup, V351 Pup, V630 Sgr, YY Tel, CQ Vel and CE-315

Woudt

Warner

2001

Monthly Notices of the Royal Astronomical Society

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The first results of a photometric survey of faint cataclysmic variables are presented. V359 Cen is an SU UMa star with a period of 112 min. Even though it is observed at quiescence, the mass‐transfer rate in this old nova may be sufficiently high that in such a short period system (with its implied small mass ratio) the disc may be excited into an elliptical shape with the result that the observed brightness modulation gives a superhump period rather than an orbital period. XZ Eri is an eclipsing dwarf nova with an orbital period (Porb) of 88.1 min. HY Lup has only slight variability. V351 Pup, the remnant of Nova Puppis 1991, has and a light curve that strongly resembles that of the magnetic Nova Cyg 1975. V630 Sgr is the first nova remnant that has both positive superhumps and eclipses . The YY Tel identification is somewhat uncertain. The correct identification for CQ Vel is provided from discovery of its flickering activity. The light curve of CE‐315, a recently discovered AM CVn star, shows similarities to that of GP Com, with no apparent orbital modulation.

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“…This possibility might be attractive because of the phase stability of the observed features. However, the quiescent magnitude of V1494 Aql more suggests a normal CV with an accretion disk (Kiss, Thomson 2000;Warner 1986), which would almost preclude the polar-type interpretation.…”

Section: Orbital Light Curvementioning

confidence: 99%

V1494 Aql: Eclipsing Fast Nova with an Unusual Orbital Light Curve

Katô¹,

Ishioka²,

Uemura³

et al. 2004

Publications of the Astronomical Society of Japan

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We present time-resolved photometry of V1494 Aql (Nova Aql 1999 No. 2) between 2001 November and 2003 June. The object is confirmed to be an eclipsing nova with a period of 0.1346138(2) d. The eclipses were present in all observed epochs. The orbital light curve shows a rather unusual profile, consisting of a bump-like feature at phase 0.6-0.7 and a dip-like feature at phase 0.2-0.4. These features were probably persistently present in all available observations between 2001 and 2003. A period analysis outside the eclipses has confirmed that these variations have a period common to the orbital period, and are unlikely interpreted as superhumps. We suspect that structure (probably in the accretion disk) fixed in the binary rotational frame is somehow responsible for this feature.

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Real Folk

Cited by 9 publications

References 0 publications

A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

High-speed photometry of faint cataclysmic variables - I. V359 Cen, XZ Eri, HY Lup, V351 Pup, V630 Sgr, YY Tel, CQ Vel and CE-315

V1494 Aql: Eclipsing Fast Nova with an Unusual Orbital Light Curve

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