Photometric study of the FUor star V 1735 Cyg (Elias 1-12)

Peneva, S.; Semkov, E.; Stavrev, K. Y.

doi:10.1007/s10509-009-0078-7

Cited by 13 publications

(22 citation statements)

References 20 publications

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“…This minimum in brightness was explained by an obscuration from a dust material ejected from the star (Kenyon et al 1991). Evidence for strong light variability in the time of set in brightness (ΔV = 1. m 2) during the period from 1986 to 1992 was reported in the photometric study of another FUor object, V1735 Cyg (Peneva et al 2009). A short drop in brightness was observed in 2009 (decrease by 0. m 4 (I) and return to its previous level) in the light curve of V733 Cep, which is also recognized as a FUor object .…”

Section: Discussionmentioning

confidence: 58%

“…outburst amplitude, association with reflection nebulae, location in star-forming regions, an F-G supergiant spectrum during outbursts, a strong LiI 6707 Å line in absorption, and CO bands in near-infrared spectra (Herbig 1977;Reipurth & Aspin 2010). Typically the decrease in brightness goes smoothly, but several events of temporary drops in brightness have been registered in the cases of V1515 Cyg (Kenyon et al 1991;Clark et al 2005), V733 Cep and V1735 Cyg (Peneva et al 2009). An important feature of FUors is the massive supersonic wind observed as a P Cyg profile most commonly for both Hα and Na I D lines.…”

Section: Introductionmentioning

confidence: 98%

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Photometric and spectroscopic variability of the FUor star V582 Aurigae

Semkov¹,

Peneva²,

Munari³

et al. 2013

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Aims. We present results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V582 Aur. Variability of the star was reported a few years ago when it was suspected as a possible FU Orionis object. Due to the small number of currently known FUors, a new object of this type is ideal target for follow-up photometric and spectroscopic observations. Methods. We carried out BVRI CCD photometric observations in the field of V582 Aur from 2009 August to 2013 February. We acquired high-, medium-, and low-resolution spectroscopy of V582 Aur during this period. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using a sequence of 14 stars in the field of V582 Aur calibrated in BVRI. Results. The pre-outburst photographic observations of V582 Aur show low-amplitude light variations typical of T Tauri stars. Archival photographic observations indicate that the increase in brightness began in late 1984 or early 1985 and the star reached the maximum level of brightness at 1986 January. The spectral type of V582 Aur can be defined as G0I with strong P Cyg profiles of Hα and Na I D lines, which are typical of FU Orionis objects. Our BVRI photometric observations show large amplitude variations (ΔV ∼ 2. m 8) during the 3.5 year period of observations. Most of the time, however, the star remains in a state close to the maximum brightness. The deepest drop in brightness was observed in the spring of 2012, when the brightness of the star fell to a level close to the pre-outburst. The multicolor photometric data show a color reversal during the minimum in brightness, which is typical of UX Ori variables. The corresponding spectral observations show strong variability in the profiles and intensities of the spectral lines (especially Hα), which indicate significant changes in the accretion rate. On the basis of photometric monitoring performed over the past three years, the spectral properties of the maximal light, and the shape of the long-term light curve, we confirm the affiliation of V582 Aur to the group of FU Orionis objects.

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Section: Discussionmentioning

confidence: 58%

Section: Introductionmentioning

confidence: 98%

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Semkov¹,

Peneva²,

Munari³

et al. 2013

A&A

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“…For some years, we have made efforts to construct the historical light curves of several other FUor and FUor-like objects such as: V1735 Cyg (Peneva et al 2009), Parsamian 21 (Semkov & Peneva 2010c), V733 Cep , and V582 Aur (Semkov et al 2011). Our results suggest that each object of this type has a characteristic long-term light curve, which distinguishes it from other objects.…”

Section: Resultsmentioning

confidence: 82%

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

Semkov

Peneva

Munari

et al. 2012

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Aims. We present new results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V2493 Cyg (HBC 722). The object has continued to undergo significant brightness variations over the past few months and is an ideal target for follow-up observations. Methods. We carried out CCD BVRI photometric observations in the field of V2493 Cyg ("Gulf of Mexico") from August 1994 to April 2012, i.e. at the pre-outburst states and during the phases of the outburst. We acquired high, medium, and low resolution spectroscopy of V2493 Cyg during the outburst. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using 15 comparison stars in the field of V2493 Cyg. Results. The pre-outburst photographic and CCD photometric observations of V2493 Cyg show low-amplitude light variations typical of T Tauri stars. The recent photometric data show a slow light decrease from October 2010 to June 2011 followed by an increase in brightness that continued until early 2012. The spectral observations of V2493 Cyg are typical of FU Orionis stars absorption spectra with strong P Cyg profiles of Hα and Na I D lines. On the basis of photometric monitoring performed over the past two years, the spectral properties at the maximal light, as well as the shape of long-term light curves, we confirm that the observed outburst of V2493 Cyg is of FU Orionis type.

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“…This minimum in brightness was attributed to obscuration caused by dust material ejected from the star (Kenyon et al 1991). Evidence of strong light variability at the time of set in brightness (ΔV = 1. m 2) were reported in the photometric study of another FUor object -V1735 Cyg (Peneva et al 2009). In 2004, the measured relatively faint red magnitude for V733 Cep (Reipurth et al 2007) can be attributed similarly to variable obscuration by dust material.…”

Section: Resultsmentioning

confidence: 83%

“…For a few objects, V1735 Cyg (Elias 1978;Peneva et al 2009), V346 Nor (Graham & Frogel 1985), and V733 Cep (Reipurth et al 2007), the presence of an optical outburst is also documented and they are labeled classical FUors. Two new suspected FUor objects with observed outbursts at optical wavelengths are reported: V582 Aurigae (Samus 2009;Munari et al 2009) and the object CSS091110, coincident with the infrared source IRAS 06068-0641 (Wils et al 2009).…”

Section: Introductionmentioning

confidence: 99%

A long-term photometric study of the FU Orionis star V 733 Cephei

Peneva

Semkov

Munari

et al. 2010

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Context. The FU Orionis candidate V733 Cep was discovered by Roger Persson in 2004. The star is located in the dark cloud L1216 close to the Cepheus OB3 association. Because only a small number of FU Orionis stars have been detected to date, photometric and spectral studies of V733 Cep are of great interest. Aims. The studies of the photometrical variability of PMS stars are very important to the understanding of stellar evolution. The main purpose of our study is to construct a long-time light curve of V733 Cep. On the basis of BVRI monitoring we also study the photometric behavior of the star. Methods. We gather data from CCD photometry and archival photographic plates. The photometric BVRI data (Johnson-Cousins system) that we present were collected from June 2008 to October 2009. To facilitate transformation from instrumental measurements to the standard system, fifteen comparison stars in the field of V733 Cep were calibrated in BVRI bands. To construct a historical light curve of V733 Cep, a search for archival photographic observations in the Wide-Field Plate Database was performed. As a result, 192 photographic plates containing the field of V733 Cep were found. Some plates were analyzed at our request to estimate the magnitude of V733 Cep.

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Photometric study of the FUor star V 1735 Cyg (Elias 1-12)

Cited by 13 publications

References 20 publications

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

A long-term photometric study of the FU Orionis star V 733 Cephei

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