A new deep minimum in the light curve of the PMS star  V 1184 Tauri (CB 34V)

Semkov, E.

doi:10.1051/0004-6361:20040142

Cited by 9 publications

(12 citation statements)

References 13 publications

(20 reference statements)

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“…The data presented in this paper are a continuation of our investigation of V 1184 Tau (Semkov 2003(Semkov , 2004(Semkov , 2006. Our first photometric and spectroscopic investigation (Semkov 2003) reveals V 1184 Tau as a possible weak-line T Tauri star (WTTS) with an amplitude of 0. m 6 (V) and spectral variability.…”

Section: Introductionmentioning

confidence: 60%

“…Our CCD photometric data (Semkov 2003(Semkov , 2004(Semkov , 2006 Another important result from our photometric study is the variation in color indices with stellar brightness. In Fig.…”

Section: Resultsmentioning

confidence: 99%

“…Our first photometric and spectroscopic investigation (Semkov 2003) reveals V 1184 Tau as a possible weak-line T Tauri star (WTTS) with an amplitude of 0. m 6 (V) and spectral variability. In our second paper (Semkov 2004), the beginning of a new deep minimum of the light curve of V 1184 Tau was reported. In the third paper (Semkov 2006), new data from the optical photometry and spectroscopy of V 1184 Tau in the period of minimum light was presented.…”

Section: Introductionmentioning

confidence: 89%

“…The technical parameters for the CCD cameras used, observational procedure, and data reduction process are described in Semkov (2003 (Semkov 2003(Semkov , 2004(Semkov , 2006, and the present paper) is plotted in Fig. 1. …”

Section: Observationsmentioning

confidence: 99%

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A long-term photometric study of V 1184 Tauri

Semkov¹,

Tsvetkov²,

Borisova³

et al. 2008

A&A

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Aims. The main purpose of our investigation is to construct the long-time light curve of the PMS star V 1184 Tau. We consider the study of the photometrical variability of PMS stars as very important for understanding stellar evolution. The unusual photometric variability of V 1184 Tau was reported in previous studies as well, but the nature of the observed deep minima is still under discussion. Methods. We present recent data from CCD photometry and from archival photographic plates. The photometric BVRI data presented in this paper were collected from November 2005 to November 2007. To construct the historical light curve of V 1184 Tau, a search for archived photographic observations in the Wide-Field Plate Database (WFPDB) was made. As a result, 412 photographic plates were found containing the field of V 1184 Tau. A part of the plates were scanned at our request and a magnitude estimation was made of V 1184 Tau. Results. Our recent photometric data suggest that the star brightness is still near the minimum. Thus the period of strong light variations that started in 2003 continues up to the present, hence more than 4 years. Our data from the archival photographic plates suggest that an unknown minimum of brightness exists in the approximate period 1980−1985. Taking all available photometric and spectroscopic data into account we must reject the hypothesis that V 1184 Tau is an FU Orionis type object. V 1184 Tau is a G type low-mass star whose spectrum is similar to WTT stars, but its photometric behavior is typical of the UX Orionis variable stars. Assuming the obscuration from orbiting dust clouds as a reason for a deep minimum, we estimate the approximate period of obscurations and the interval between two deep minima. Our calculations give a 25−28 year period between the two minima and approximately 8−10 year duration of the minima.

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Section: Introductionmentioning

confidence: 60%

“…Our CCD photometric data (Semkov 2003(Semkov , 2004(Semkov , 2006 Another important result from our photometric study is the variation in color indices with stellar brightness. In Fig.…”

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 89%

Section: Observationsmentioning

confidence: 99%

See 2 more Smart Citations

A long-term photometric study of V 1184 Tauri

Semkov¹,

Tsvetkov²,

Borisova³

et al. 2008

A&A

Self Cite

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show abstract

“…The photometric and spectroscopic study presented in our first paper (Semkov 2003) reveals V1184 Tau as a possible WTT star with an amplitude of 0. m 5 (I) and spectral variability. In our second paper (Semkov 2004), the beginning of a new very deep minimum in brightness of V1184 Tau was reported. In the third paper from our study (Semkov 2006), new data from optical photometry and spectroscopy of V1184 Tau in the period during the deep minimum are reported.…”

Section: Introductionmentioning

confidence: 85%

The pre-main-sequence star V1184 Tauri (CB 34V) at the end of prolonged eclipse

Semkov

Peneva

Ibryamov

2015

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Aims. V1184 Tau (CB 34V) lies in the field of the Bok globule CB 34 and was discovered as a large amplitude variable in 1993. According to the first hypothesis of the variability of the star, it is a FU Orionis candidate erupted between 1951 and 1993. During subsequent observations, the star manifests large amplitude variability interpreted as obscuration from circumstellar clouds of dust. We included V1184 Tau (CB 34V) in our target list of highly variable pre-main-sequence stars to determine the reasons for the variations in the brightness of this object. Methods. Data from BVRI photometric observations of the young stellar object V1184 Tau, obtained in the period 2008−2015, are presented in the paper. These data are a continuation of our optical photometric monitoring of the star began in 2000 and continuing to date. The photometric observations of V1184 Tau were performed in two observatories with two medium-sized and two small telescopes. Results. Our results indicate that during periods of maximum light the star shows characteristics typical of T Tauri stars. During the observed deep minimum in brightness, however, V1184 Tau is rather similar to UX Orionis objects. The deep drop in brightness began in 2003 ended in 2015 as the star has returned to maximum light. The light curve during the drop is obviously asymmetric as the decrease in brightness lasts two times longer than the rise. The observed colour reverse on the colour-magnitude diagrams is also confirmation of obscuration from circumstellar clouds of dust as a reason for the large amplitude variability in the brightness.

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