An Unusual Eclipse of a Pre-Main-Sequence Star in IC 348

Cohen, Roger E.; Herbst, W.; Williams, Eric

doi:10.1086/379275

Cited by 17 publications

(27 citation statements)

References 16 publications

(25 reference statements)

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“…Only a few PMS objects have been found to show eclipses such as KH 15D (Hamilton et al 2001;Herbst et al 2002) or HMW 15 (Cohen et al 2003). The eclipsing PMS star KH 15D varies with amplitude of 3-4 mag and a period of 48.36 days.…”

Section: Discussionmentioning

confidence: 99%

“…The unique PMS object HMW 15, found in the field of IC 348, has amplitude of observed obscuration 0. m 66 and duration of eclipse 3.5 years which is the longest value of any known eclipsing variables. According to Cohen et al (2003) an eclipse of one component of a binary star by an optically thick cloud is the most probable explanation of the eclipse. The exact determination of the eclipse parameters is necessary in order to choose which scenario explains better the variability of V 1184 Tau. An open question is the observed spectral variability of V 1184 Tau.…”

Section: Discussionmentioning

confidence: 99%

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

Semkov

2004

A&A

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Abstract. We present results from optical photometry of the pre-main sequence star V 1184 Tau. The star is associated with the Bok globule CB 34 and it was considered as a FUOR candidate in previous studies. The analysis of the photometric data suggests that V 1184 Tau shows two types of variability produced (1) by the presence of large cool photospheric spots and (2) by occultation from circumstellar clouds of dust or from an orbiting extended body. The behavior of the V − I index indicates that the star becomes redder towards minimum light, but from a certain turning point it gets bluer fading further. The possible scenarios to explain the observed eclipse are briefly discussed.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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

Semkov

2004

A&A

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“…Comprehensive photometric monitoring of V718 Per by Cohen et al (2003) revealed a very unusual eclipse in this object. They detected an extremely long and smooth eclipse (t ecl ≈ 3.5 yrs and an eclipse depth of ∼0.7 m ), and earlier scattered photometric data suggested that these eclipses may be recurrent (see Cohen et al 2004).…”

Section: Introductionmentioning

confidence: 91%

The unusual pre-main-sequence star V718 Persei (HMW 15)

Гринин¹,

Stempels²,

Gahm³

et al. 2008

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Context. The remarkable pre-main-sequence object V718 Per (HMW 15, H187) in the young cluster IC 348 periodically undergoes long-lasting eclipses caused by variable amounts of circumstellar dust in the line-of-sight to the star. It has been speculated that the star is a close binary and similar to another unusual eclipsing object, KH 15D. Aims. We have submitted V718 Per to a detailed photometric and spectroscopic study to investigate how regular the recurrent eclipses are, to find out more about the properties of the stellar object and the occulting circumstellar material, and to look for signatures of a possible binary component. Methods. V718 Per was monitored photometrically from the optical to the near-infrared (NIR). We also obtained high-resolution optical spectra with the Keck telescope at minimum as well as at maximum brightness. We derived the fundamental photospheric parameters of this star by comparing with synthetic spectra. Results. Our photometric data show that the eclipses are very symmetric and persistent, and that the extinction law of the foreground occulting dust deviates only little from what is expected for "normal" interstellar material. The stellar parameters of V718 Per indicate a primordial abundance of Li and a surface temperature of T eff ≈ 5200 K. Remarkably, the in-eclipse spectrum shows a significant broadening of the photospheric absorption lines, as well as a slightly lower stellar surface temperature. In addition, weak emission components appear in the absorption lines of Hα and the Ca II IR triplet lines. We did not detect any signs of atomic or molecular features related to the occulting body in the in-eclipse spectrum. We also found no evidence of any radial velocity changes in V718 Per to within about ±80 m s −1 , which for an edge-on system corresponds to a maximum companion mass of ∼6 M Jup . Conclusions. Our observations suggest that V718 Per is a single star, and thus very different from the related binary system KH 15D. We conclude that V718 Per is surrounded by an edge-on circumstellar disk with an irregular mass distribution orbiting at a distance of 3.3 AU from the star, presumably at the inner disk edge. To produce the prolonged eclipses, the occulting feature must extend along more than half of the inner disk edge. The change in stellar surface temperature and the emission line activity observed could be related to spot activity. We ascribe the broadening of photospheric absorption lines during the eclipse to forward scattering of stellar light in the circumstellar dust feature.

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“…In an earlier photometric study of the cluster IC 348 Herbig [6] took note of the variability in the brightness of H 187, but an extended eclipse of the sort detected by Cohen et al [4,5] had not been observed before. Thus it is impossible to say whether these reductions in brightness are a periodic process typical of an eclipsing binary system.…”

Section: Introductionmentioning

confidence: 98%

“…For example, for the star KH 15D (Kerns and Herbst [1], Hamilton et al [2], Barsunova et al [3]) the duration of the eclipse is roughly 1/3 of the period and is increasing with time. Cohen et al [4,5] have recently observed an unusual reduction in the brightness of the weak T Tauri star (WTTS) H 187 in the IC 348 cluster. (A chart of the neighborhood of this object is shown in Fig.…”

Section: Introductionmentioning

confidence: 99%