Minimum on the light curve of the classical symbiotic star AS 338 in 1999

Kolotilov, E. A.; Mikolajewska, I.; Marrese, P. M.; Munari, U.; Shugarov, S. Yu.; Yudin, B. F.

doi:10.1134/1.1336862

Cited by 19 publications

(35 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The photometer's parameters and observing techniques were described by Kolotilov et al (1998). Spectroscopic observations were acquired with the 2.6-m G.A.…”

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

Four states of the recurrent symbiotic nova V407 Cyg

et al. 2013

View full text Add to dashboard Cite

show abstract

“…The photometer's parameters and observing techniques were described by Kolotilov et al (1998). Spectroscopic observations were acquired with the 2.6-m G.A.…”

Section: Observationsmentioning

confidence: 99%

“…Such spectra were obtained on October 10, 1952 (Herbig 1960) and May 29, 1993(Kolotilov et al 1998). H I emission lines are observed in the spectra of some ordinary (non-symbiotic) Miras soon after their brightness maxima.…”

Section: Passive Statementioning

confidence: 99%

Four states of the recurrent symbiotic nova V407 Cyg

et al. 2013

View full text Add to dashboard Cite

show abstract

“…where the original B-band ephemeris of Meinunger (1966) was found to be the best performing one for the R data and the Kolotilov et al (1998) ephemeris the best for the J data. They are however not satisfactory for I and K data, for which we determined new periodicities with converging results by different techniques (Fourier and phase dispersion minimization).…”

Section: V407 Cygmentioning

confidence: 99%

“…On the basis of marked spectral changes and the emission line Table 2 and J and K data from Kolotilov et al (1998) spectrum, Munari et al (1999) suggested a possible symbiotic nature for this object. Our B and V data in Table 2 reveal a variability of significant amplitude, but the resulting lightcurve is disappointingly restricted to a narrow range.…”

Section: V335 Vul Fg Ser Draco C-1mentioning

confidence: 99%

“…If the presence of the accreting and outbursting white dwarf companion inhibits the formation of all but an optically thin circumstellar dust shell (Kolotilov et al 1998), then V407 Cyg would allow an unobstructed view of the central star of an OH/IR source. The dust could partially form and survive only in the shadow cone produced by the Mira itself, which blocks the destroying action of the white dwarf hard radiation field.…”

Section: V407 Cygmentioning

confidence: 99%

See 1 more Smart Citation

Symbiotic stars on Asiago archive plates. II

Munari

Jurdana-Šepić

2002

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. The Asiago photographic archive has been searched for plates containing the symbiotic stars Hen 2-468, QW Sge, LT Del, V407 Cyg, K 3-9, V335 Vul, FG Ser and Draco C-1. A total of 635 plates imaging the program stars have been found and the brightness estimated using the Henden & Munari (2000) UBV(RI)C photometric sequences. These historical data have allowed for the first time the determination of the orbital periods of Hen 2-468 (774 days) and QW Sge (390.5 days), a significant improvement in the orbital period of LT Del (465.6 days) and for V407 Cyg an evaluation of the Mira's pulsation period and complex lightcurve shape in the red (R and I bands). Some previously unknown outbursts have been discovered too.

show abstract

Spectral variations of the symbiotic star V407 Cygni around light maximum of the secondary Mira variable in 2012

Iijima

Naito

2017

A&A

View full text Add to dashboard Cite

Context. The outburst of the symbiotic recurrent nova V407 Cyg in 2010 has been studied by numerous authors. On the other hand, its spectral variations in the quiescent stage have not been well studied yet. This paper is probably the first report for the relation between the pulsation of the secondary Mira variable and the temperature of the primary hot component for V407 Cyg. Aims. The spectral variation in the post-outburst stage has been monitored to study the properties of this object. In the course of this work, we found some unexpected spectral variations around the light maximum of the secondary Mira variable in 2012. The relation between the mass transfer in the binary system and the pulsation of the secondary Mira variable is studied. Methods. High-and low-resolution optical spectra obtained at the Astronomical Observatories at Asiago were used. The photometric data depend on the database of the VSNET. Results. The secondary Mira variable reached its light maximum in 2012, when an absorption spectrum of a late-M-type giant developed and the emission line of Hδ became stronger than those of Hβ and Hγ, which are typical spectral features of Mira variables at light maxima. On the other hand, intensity ratios to Hβ of the emission lines of He I, He II, [Fe VII], etc., which obviously depended on the temperature of the hot component, rapidly varied around the light maximum. The intensity ratios started to decrease at phase about 0.9 of the periodical light variation of the Mira variable. This phenomenon suggests that the mass transfer rate, as well as the mass accretion rate onto the hot component, decreased according to the contraction of the Mira variable. However, these intensity ratios somewhat recovered just on the light maximum: phase 0.99. There might have occurred a temporal mass loss from the Mira variable at that time. The intensity ratios decreased again after the light maximum, then recovered and returned to the normal level at phase about 0.1. Since the mass transfer rate seems to have been closely related to the pulsation of the secondary component, the mass transfer in this binary system was likely due to a normal Roche-lobe overflow. If this is the case, the orbital period should be shorter than five years. Each of the Na I D1 and D2 lines had five emission and one absorption components around the light maximum. It seems that there were two pairs of mass outflows from the Mira variable with velocities of ±79 km s −1 and ±44 km s −1 . These velocities were much higher than those of mass loss from usual Mira variables.

show abstract

Minimum on the light curve of the classical symbiotic star AS 338 in 1999

Cited by 19 publications

References 2 publications

Four states of the recurrent symbiotic nova V407 Cyg

Four states of the recurrent symbiotic nova V407 Cyg

Symbiotic stars on Asiago archive plates. II

Spectral variations of the symbiotic star V407 Cygni around light maximum of the secondary Mira variable in 2012

Contact Info

Product

Resources

About