Spectroscopic Variability of the UXOR Star RR Tauri

Rodgers, Bernadette; Wooden, D. H.; Гринин, В. П.; Shakhovsky, Dmitry; Natta, A.

doi:10.1086/324213

Cited by 35 publications

(38 citation statements)

References 19 publications

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“…Evidence for outflowing gas in SAGE050756-703453 can be seen in its P-Cygni emission line profiles (Figure 2) but no indication of infall is seen. However, inverse P-Cygni profiles are generally seen only near maximum light (Rodgers et al 2002). But the infall rate inferred by this model fits well with the estimated absolute bolometric luminosity of SAGE050756-703453.…”

Section: Discussionsupporting

confidence: 68%

“…The line ratios of the Ca II IR triplet are close to 1:1:1 in both stars indicating that the gas is optically thick. The wings of the Balmer lines in RR Tau seem to be broader than those in SAGE050756-703453 possibly indicating that RR Tau may be less luminous (Rodgers et al 2002). Another indication that SAGE050756-703453 is luminous is the strength of the O I λλ7774, 8446 triplets (Mendoza 1971).…”

Section: Discussionmentioning

confidence: 99%

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HERSCHELOBSERVATIONS OF A NEWLY DISCOVERED UX Ori STAR IN THE LARGE MAGELLANIC CLOUD

Clayton

Sargent

Boyer

et al. 2010

ApJ

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The LMC star, SSTISAGE1C J050756.44-703453.9, was first noticed during a survey of EROS-2 lightcurves for stars with large irregular brightness variations typical of the R Coronae Borealis (RCB) class. However, the visible spectrum showing emission lines including the Balmer and Paschen series as well as many Fe II lines is emphatically not that of an RCB star. This star has all of the characteristics of a typical UX Ori star. It has a spectral type of approximately A2 and has excited an H II region in its vicinity. However, if it is an LMC member, then it is very luminous for a Herbig Ae/Be star. It shows irregular drops in brightness of up to 2 mag, and displays the reddening and "blueing" typical of this class of stars. Its spectrum, showing a combination of emission and absorption lines, is typical of a UX Ori star that is in a decline caused by obscuration from the circumstellar dust. SSTISAGE1C J050756.44-703453.9 has a strong IR excess and significant emission is present out to 500 µm. Monte Carlo radiative transfer modeling of the SED requires that SSTISAGE1C J050756.44-703453.9 has both a dusty disk as well as a large extended diffuse envelope to fit both the mid-and far-IR dust emission. This star is a new member of the UX Ori subclass of the Herbig Ae/Be stars and only the second such star to be discovered in the LMC.

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Section: Discussionsupporting

confidence: 68%

Section: Discussionmentioning

confidence: 99%

HERSCHELOBSERVATIONS OF A NEWLY DISCOVERED UX Ori STAR IN THE LARGE MAGELLANIC CLOUD

Clayton

Sargent

Boyer

et al. 2010

ApJ

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“…These extinction events are usually deeper, though this may be an observational bias. Rodgers et al 2002) are likely caused by the interstellar medium rather than the disk. Dust heating and processing within the disk of GI Tau must have destroyed the complex molecules that cause these bands.…”

Section: The Extinction Curve Of the Dips Of Gi Taumentioning

confidence: 99%

Star–Disk Interactions in Multiband Photometric Monitoring of the Classical T Tauri Star GI Tau

Guo

Herczeg

Jose

et al. 2018

ApJ

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The variability of young stellar objects is mostly driven by star-disk interactions. In long-term photometric monitoring of the accreting T Tauri star GI Tau, we detect extinction events with typical depths of DṼ 2.5 mag that last for days to months and often appear to occur stochastically. In 2014-2015, extinctions that repeated with a quasi-period of 21 days over several months are the first empirical evidence of slow warps predicted by magnetohydrodynamic simulations to form at a few stellar radii away from the central star. The reddening is consistent with =  R 3.85 0.5 V and, along with an absence of diffuse interstellar bands, indicates that some dust processing has occurred in the disk. The 2015-2016 multiband light curve includes variations in spot coverage, extinction, and accretion, each of which results in different traces in color-magnitude diagrams. This light curve is initially dominated by a month-long extinction event and a return to the unocculted brightness. The subsequent light curve then features spot modulation with a 7.03 day period, punctuated by brief, randomly spaced extinction events. The accretion rate measured from U-band photometry ranges from´-1.3 10 8 to´-1.1 10 10 M e yr −1 (excluding the highest and lowest 5% of high-and low-accretion rate outliers), with an average of4.7 -10 9 M e yr −1 . A total of 50% of the mass is accreted during bursts of >´-12.8 10 9 M e yr -1, which indicates limitations on analyses of disk evolution using single-epoch accretion rates.

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“…(This figure is available in color in electronic form.) Rodgers et al (2002), which provides this ratio under the assumption of a stellar and a circumstellar contribution to the observed flux; the circumstellar contribution is caused by a spherical occulting cloud and a more extended envelope. In our zero order approach we neglect the extended envelope, and we assume a small optical depth and black-body emission for the spherical occulting cloud.…”

Section: Origin Of the Circumstellar Gasmentioning

confidence: 99%

A dynamical study of the circumstellar gas in UX Orionis

Mora

Natta²,

Eiroa³

et al. 2002

A&A

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Abstract. We present the results of a high spectral resolution (λ/∆λ = 49 000) study of the circumstellar (CS) gas around the intermediate mass, pre-main sequence star UX Ori. The results are based on a set of 10échelle spectra covering the spectral range 3800-5900 Å, monitoring the star on time scales of months, days and hours. A large number of transient blueshifted and redshifted absorption features are detected in the Balmer and in many metallic lines. A multigaussian fit is applied to determine for each transient absorption the velocity, v, dispersion velocity, ∆v, and the parameter R, which provides a measure of the absorption strength of the CS gas. The time evolution of those parameters is presented and discussed. A comparison of intensity ratios among the transient absorptions suggests a solar-like composition of the CS gas. This confirms previous results and excludes a very metal-rich environment as the cause of the transient features in UX Ori. The features can be grouped by their similar velocities into 24 groups, of which 17 are redshifted and 7 blueshifted. An analysis of the velocity of the groups allows us to identify them as signatures of the dynamical evolution of 7 clumps of gas, of which 4 represent accretion events and 3 outflow events. Most of the events decelerate at a rate of tenths of m s −2 , while 2 events accelerate at approximately the same rate; one event is seen experiencing both an acceleration and a deceleration phase and lasts for a period of few days. This time scale seems to be the typical duration of outflowing and infalling events in UX Ori. The dispersion velocity and the relative aborption strength of the features do not show drastic changes during the lifetime of the events, which suggests they are gaseous blobs preserving their geometrical and physical identity. These data are a very useful tool for constraining and validating theoretical models of the chemical and physical conditions of CS gas around young stars; in particular, we suggest that the simultaneous presence of infalling and outflowing gas should be investigated in the context of detailed magnetospheric accretion models, similar to those proposed for the lower mass T Tauri stars.

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Spectroscopic Variability of the UXOR Star RR Tauri

Cited by 35 publications

References 19 publications

HERSCHELOBSERVATIONS OF A NEWLY DISCOVERED UX Ori STAR IN THE LARGE MAGELLANIC CLOUD

HERSCHELOBSERVATIONS OF A NEWLY DISCOVERED UX Ori STAR IN THE LARGE MAGELLANIC CLOUD

Star–Disk Interactions in Multiband Photometric Monitoring of the Classical T Tauri Star GI Tau

A dynamical study of the circumstellar gas in UX Orionis

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