Beobachtungsergebnisse der Berliner Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV)

Braune, W.; Hübscher, J.; Mundry, Eberhard

doi:10.1002/asna.19772980210

Cited by 7 publications

(3 citation statements)

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“…Most of the published times of maxima were collected in the GEOS 3 database (Graff 1922;Waterfield 1927;Luizet 1930;Ivanov 1930a,b;Chudovichev 1930;Dubiago 1930;Blazhko 1935;Lange 1935Lange , 1969Kleissen 1939;Batyrev 1950Batyrev , 1962Alania 1956;Guriev 1958;Mandel 1960;Fitch et al 1966;Epstein 1969;Tsesevich 1969;Kanischeva & Lange 1971;Lange et al 1976;Braune et al 1977;Liu & Janes 1989;ESA 1997;Vandenbroere 1997Vandenbroere , 1998Vandenbroere , 1999Vandenbroere , 2001Vandenbroere , 2003Vandenbroere , 2005Gensler 1998;Agerer & Huebscher 2000Huebscher 2000Huebscher , 2003Huebscher , 2005Agerer et al 2001;Huebscher et al 2005;Le Borgne 2004;Le Borgne et al 2005, 2006Wils et al 2006). A few additional maxima times of Waterfield (1927) and Graff (1922) were also considered.…”

Section: (O-c) Maxmentioning

confidence: 99%

The Blazhko behaviour of RR Geminorum II

Sódor¹,

Szeidl²,

Jurcsik³

2007

A&A

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Context. RR Gem is one of the few Blazhko RR Lyrae that has photometric observations available extended enough to study the long-term courses of its pulsation and modulation properties in detail. Aims. We investigate the pulsation and modulation properties and the relations between them in RR Gem using photometric observations from the past 70 years in order to gain further insight into the nature of the Blazhko modulation. Methods. We studied the photographic, photoelectric, and CCD light curves obtained at the Konkoly Observatory and other authors' published maxima observations. Detailed analysis of the light curves, maximum brightness, and O-C data are carried out. Results. RR Gem showed modulation most of the time it was observed. The modulation amplitude showed strong variations from the undetectable level (less than 0.04 mag in maximum brightness) to about 0.20 mag. The amplitudes of the amplitude and phase modulations showed parallel changes, thus the total "power" of the modulation have changed during the past 70 years. Parallel changes in the pulsation and modulation periods occur with a dP mod /dP puls = 1.6 ± 0.8 × 10 3 ratio. We also detected 0.05−0.1 mag changes in the mean maximum brightness and mean pulsation amplitude.

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Section: (O-c) Maxmentioning

confidence: 99%

The Blazhko behaviour of RR Geminorum II

Sódor¹,

Szeidl²,

Jurcsik³

2007

A&A

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“…Constructing the O − C diagram of the pulsation we also utilized maximum times from the literature when no photometric data were given Agerer & Hübscher 2002, 2003Ahnert 1961;Aubaud 1991;Braune & Hübscher 1967Braune & Mundry 1982;Braune, Hübscher & Mundry 1970, 1972, 1977, 1979Dombrovski 1935;Fitch, Wisniewski & Johnson 1966;Geyer 1961;Hübscher 2000Hübscher , 2001Hübscher , 2003Hübscher , 2005Hübscher et al 1994Hübscher et al , 1998Hübscher et al , 1999Hübscher & Lichtenknecker 1988;Hübscher & Mundry 1984;Hübscher, Agerer & Wunder 1991, 1992, 1995Hübscher, Lichtenknecker & Meyer 1987;Hübscher, Lichtenknecker & Wunder 1989, 1990Hübscher, Paschke & Walter 2005;Lange & Kanishcheva 1961;Le Borgne, Klotz & Boër 2004Solo-viev 1936Solo-viev , 1941Tsesevich 1969;Vandenbroere 1997Vandenbroere , 1999Vandenbroere , 2001Vandenbroere , 2005.…”

Section: The Dataunclassified

The Blazhko behavior of RV UMa

Hurta

2007

Astron Nachr

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RV UMa is one of the most extensively studied RR Lyrae stars showing Blazhko modulation. Its photometric observations cover more than 90 years. The published photoelectric observations of RV UMa obtained at the Konkoly Observatory (Kanyo, 1976) were re-considered and completed with previously unpublished data. During the time interval of the observations the periods of both the pulsation and the modulation varied within the ranges of 0.000007 and 0.9 days, respectively. We have found a definite but not strict inverse relation between the pulsation and modulation periods of RV UMa.Comment: 4 pages, 5 figures, accepted for publication in A

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“…N min I : : : : : : : : : : : : : : : : : : : Szafraniec 1955;(8) Tshuprina 1957;(9) Szafraniec 1956;(10) Szafraniec 1958;(11) Busch 1975;(12) Winiarski 1972;(13) Braune et al 1977;(14) Diethelm 1975;(15) Diethelm 1976;(16) Diethelm 1983;(17) Lacy et al 1995;(18) Diethelm 1992;(19) Lacy & Fox 1994. Table 5. Absolute photometry of GG Ori and comparison stars.…”

Section: Appendixunclassified

Absolute Dimensions of the Unevolved B-Type Eclipsing Binary GG Orionis

Torres

Lacy

Claret

et al. 2000

The Astronomical Journal

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We report extensive differential V -band photometry and high-resolution spectroscopy for the 1.14 day, detached, double-lined eclipsing binary BT Vul (F0+F7). Our radial-velocity monitoring and light curve analysis lead to absolute masses and radii of M 1 = 1.5439 ± 0.0098 M N ⊙ and R 1 = 1.536 ± 0.018 R N ⊙ for the primary, and M 2 = 1.2196 ± 0.0080 M N ⊙ and R 2 = 1.151 ± 0.029 R N ⊙ for the secondary. The effective temperatures are 7270 ± 150 K and 6260 ± 180 K, respectively. Both stars are rapid rotators, and the orbit is circular. A comparison with stellar evolution models from the MIST series shows excellent agreement with these determinations, for a composition of [Fe/H] = +0.08 and an age of 350 Myr. The two components of BT Vul are very near the zero-age main sequence.

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Beobachtungsergebnisse der Berliner Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV)

Cited by 7 publications

References 0 publications

The Blazhko behaviour of RR Geminorum II

The Blazhko behaviour of RR Geminorum II

The Blazhko behavior of RV UMa

Absolute Dimensions of the Unevolved B-Type Eclipsing Binary GG Orionis

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