Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau

We report the results of optical spectroscopic monitoring observations of a T Tauri star, V409 Tau. A previous photometric study indicated that this star experienced dimming events due to the obscuration of light from the central star with a distorted circumstellar disk. We conducted medium-resolution (R ~10,000) spectroscopic observations with 2-m Nayuta telescope at Nishi-Harima Astronomical Observatory. Spectra were obtained in 18 nights between November 2015 and March 2016. Several absorption lines such as Ca I and Li, and the Hαemission line were confirmed in the spectra. The Ic-band magnitudes of V409 Tau changed by approximately 1 magnitude during the observation epoch. The equivalent widths of the five absorption lines are roughly constant despite changes in the Ic-band magnitudes. We conclude that the light variation of the star is caused by the obscuration of light from the central star with a distorted circumstellar disk, based on the relationship between the equivalent widths of the absorption lines and the Ic-band magnitudes. The blue component of the Hαemission line was dominant during the observation epoch, and an inverse P Cygni profile was observed in eight of the spectra. The time-variable inverse P Cygni profile of the Hαemission line indicates unsteady mass accretion from the circumstellar disk to the central star.

Spin evolution of classical T Tauri stars

Classical T Tauri stars (hereinafter CTTS) are protostars formed by collapse of molecular clouds. As they evolve towards the main sequence, CCTS accrete from the circumstellar matter and contract due to self-gravitation. Mass accretion and gravitational contraction can accelerate the spin velocities of CTTS up to break-up (～300—400km·s)

T Tauri型星及其类太阳活动

该文从低质量恒星的形成、主序前演化、多波段测光和光谱观测及研究等方面,着重介绍类太阳恒星的主序前演化特性、T Tauri型星的分类、光变特性和光谱特征、弱发射线T Tauri型星(WTTS)的光学证认,以及其光度变化与发射线轮廓变化间的内在联系。相关研究对于认识类太阳恒星的形成、早期及后续演化、类太阳活动特性和活动机理等具有重要意义。另外,该文对国内外T Tauri型星观测和研究的现状进行了介绍,同时也给出了国内学者近年来在相关领域进行观测研究的部分结果。

T Tauri型星的多波段测光研究

为证明主序前星向零龄主序星演化过程中自转加快的理论预期,创新性的由强X-ray源选取11颗弱发射线T Tauri型星,并进行了多波段的测光观测.应用PDM和付理叶分析两种方法获得了其中6颗的光变周期,且多数短于1天.结果证明主序前恒星随星龄的增加自转加快,及金牛-御夫恒星形成区其星云中心的恒星明显的较外侧的恒星更为年轻.

Spectroscopic Survey of Hα Emission Line Stars Associated with Bright Rimmed Clouds

The results of a spectroscopic survey of Hα emission line stars associated with fourteen bright rimmed clouds are presented. Slit-less optical spectroscopy was carried out with the Inter University Centre for Astronomy and Astrophysics (IUCAA) 2 m telescope and IUCAA Faint Object Spectrograph and Camera (IFOSC). Hα emission line was detected from 173 objects. Among them 85 objects have a strong Hα emission line with its equivalent width larger than 10 ?. Those are classical T Tauri stars. 52 objects have a weak Hα emission line with its equivalent width less than 10 ? and do not show intrinsic near-infrared excess. Those are weak-line T Tauri stars. On the other hand, 36 objects have a weak Hα emission line (?), although they show intrinsic near-infrared excess. Such objects are not common in low-mass star forming regions. Those are misfits of the general concept on formation process of a low-mass star, in which it evolves from a classical T Tauri star to a weak-line T Tauri star. Those might be weak-line T Tauri stars with a flared disk in which gas is heated by ultraviolet radiation from a nearby early-type star. Alternatively, we propose pre-transitional disk objects as their evolutional stage.

Discovery of Three Variable Stars in Direction toward NGC 4565

We present the results of a variable star search in a field next to the edge-on galaxies NGC 4565 from the archive data of Beijing-Arizona-Taibei-Connecticut Multicolor Sky Survey. Three new variable stars were discovered. Based on spectra obtained from the 2.16m NAOC telescope, we identify two of these as RR Lyr stars and one as a special T Tauri star.

A long-term UBVRI photometric study of the pre-main sequence star V350 Cep

Results from UBVRI optical photometric observations of the pre-main se- quence star V350 Cep during the period 2004-2014 are presented. The star was dis- covered in 1977 due to its remarkable increase in brightness by more than 5 mag （R）. In previous studies, V350 Cep was considered to be a potential FUor or EXor eruptive variable. Our data suggest that during the period of observations the star maintains its maximum brightness with low amplitude photometric variations. Our conclusion is that V350 Cep was probably an intermediate object between FUors and EXors, similar to V1647 Ori.

Long-term BV RI photometric light curves of 15 PMS stars in the star-forming region IC 5070

This paper reports results from the multicolor photometric observations of 15 pre-main sequence stars collected in the period September 2010-October 2017. The stars from our study are located in the star-forming HII region IC 5070. These objects were previously detected as either emission line stars, flare stars, T Tauri variables or Herbig Ae/Be stars. Photometric observations, especially concerning the long-term behavior of the objects, are missing in the literature. We present the first photometric monitoring for all stars from our study. The analysis of the obtained BV RI photometric data allows us to draw the conclusion that all investigated objects are variable stars. In the case of LkHα 146,we identified previously unknown periodicity in its photometric variability.

Long-term photometric behavior of the PMS stars V977 Cep and V982 Cep in the vicinity of NGC 7129

Long-term BVRI photometric light curves of the pre-main sequence stars V977 Cep and V982 Cep during the period from 2000 October to 2016 August are presented. The stars are located in the vicinity of the reflection nebula NGC 7129. Our photometric data show that both stars exhibit strong photometric variability in all optical passbands, which is typical for Classical T Tauri stars. Using our observational data we analyze the reasons for the observed brightness variations. In the case of V977 Cep we identify previously unknown periodicity in its light curve.

BV(RI )c photometric study of three variable PMS stars in the field of V733 Cephei

This paper reports results from the first long-term BV(RI)c photometric CCD observations of three variable pre-main-sequence stars collected during the period from February 2007 to January 2020. The investigated stars are located in the field of the PMS star V733 Cep within the Cepheus OB3 association. All stars from our study show rapid photometric variability in all-optical passbands. In this paper, we describe and discuss the photometric behavior of these stars and the possible reasons for their variability. In the light variation of two of the stars, we found periodicity.

Long-term Photometric Study of the Pre-main Sequence Star V1180 Cas

In this paper results from the optical photometric observations of the pre-main sequence star V1180 Cas are reported.The star is a young variable associated with the dark cloud Lynds 1340,located at a distance of 600 pc from the Sun in the star-forming region in Cassiopeia.V1180 Cas shows large amplitude variability,interpreted as a combination of accretion-induced and extinction-driven effects.Our data from VRI CCD photometric observations of the star were collected from September 2011 to February 2022.During our monitoring,we recorded several brightness dips with large amplitudes of up to 5 mag(I band).At the same time,increases in brightness over periods of several weeks have also been recorded.In this paper,we compare the photometric data obtained for V1180 Cas with observations of other low-mass pre-main sequence objects.

Long-term V(RI) CCD photometry of pre-main-sequence stars in the association Cepheus OB3

Results from optical CCD photometric observations of 13 pre-main-sequence stars collected during the period from February 2007 to November 2020 are presented.These stars are located in the association Cepheus OB3,in the field of the young star V733 Cephei.Photometric observations,especially concerning the long-term variability of the stars,are missing in the literature.We present the first longterm V(RI)c monitoring for them,that cover 13 years.Results from our study indicate that all of the investigated stars manifest strong photometric variability.The presented paper is a part of our program for the photometric study of pre-main-sequence stars located in active star-forming regions.

Spectral study of V565 Mon: probable FU Ori-like or chemically peculiar star

We present a detailed spectroscopic study of pre-main sequence star V565 Mon,which is the illuminating star of the Parsamian 17 cometary nebula.Observations were performed with the 2.6 m telescope in Byurakan Astrophysical Observatory on 2018 February 15.Radial velocities and equivalent widths of the most prominent lines of V565 Mon are presented.We build the spectral energy distribution and estimate the main parameters of the star,for example the obtained bolometric luminosity of V565 Mon is L_(V565)≈130 L_(⊙).Considering all features of V565 Mon,we come to the conclusion that this young intermediate-mass star belongs to some intermediate class between T Tau and HAeBe stars.Very unusual for a young star is the presence of strong absorption BaⅡlines in the spectrum.Possible explanations on this issue are discussed.Hence,we think that V565 Mon is a unique example,which can help to understand some open questions involved in the problem of nucleosynthesis in young stars.

金牛T型星的红外光谱

给出２６ 个金牛Ｔ 型星的ＩＲＡＳ低分辨率红外光谱．根据这些光谱讨论了它们有关的性质和所处环境．分析发现硅酸盐尘埃在金牛Ｔ

金牛T型星LkH_α120的Raman谱

最近,Raman散射被成功地用来解释某些天体的谱线形成,Raman散射在天体物理中有着广泛的应用。本文考查了金牛T型星LkH_α120的谱线资料,并估算了Raman散射的截面及谱线的强度,发现金牛T型星LkH_α120的未被证认的谱线:λλ4200.9,5098.1 5613.9,5768.0,5859.0,6633.5,6667.0,7500.0A很可能是FeI,FeII线系被H原子、H_2分子和CO分子散射后所产生的Raman谱。

金牛T星在慢引力收缩阶段抛射物质和引力收缩作用下质量和半径的演化时标及其对自转角速度变化的影响

研究了带有引力能源和抛射物质的引力收缩星如金牛T星处于慢引力收缩阶段后,在抛射物质和引力收缩联合作用下对质量和半径的改变及其对自转角速度变化产生的影响。给出了质量和半径随时间演变的联立微分方程组及其解。利用解计算了金牛T星的质量和半径的演化时标以及对自转角速度变化产生的影响。给出数值结果,并讨论了理论和数值结果。

Ionization of protoplanetary disks by galactic cosmic rays,solar protons,and supernova remnants

Galactic cosmic rays and solar protons ionize the present terrestrial atmosphere,and the air showers are simulated by well-tested Monte-Carlo simulations,such as PHITS code.We use the latest version of PHITS to evaluate the possible ionization of protoplanetary disks by galactic cosmic rays（GCRs）,solar protons,and by supernova remnants.The attenuation length of GCR ionization is updated as 118 g cm^-2,which is approximately 20% larger than the popular value.Hard and soft possible spectra of solar protons give comparable and 20% smaller attenuation lengths compared with those from standard GCR spectra,respectively,while the attenuation length is approximately 10% larger for supernova remnants.Further,all of the attenuation lengths become 10% larger in the compound gas of cosmic abundance,e.g.128 g cm^-2 for GCRs,which can affect the minimum estimate of the size of dead zones in protoplanetary disks when the incident flux is unusually high.

Variability of emission lines in the optical spectra of the Herbig Be binary system HD 200775

In our previous papers we have improved the value of the orbital period of the binary Herbig Be star HD 200775 and showed that the [O I] and Si II 6347 and 6371 ?A emission lines displayed variations which correlate with the orbital period. In this paper we provide evidences that other broad emission lines of metals in the spectra of HD 200775 also exhibit variability, which is probably related to the orbital cycle of the binary. Analysis was performed based on the high-resolution spectral data collected over a time span of 6 years at the Kourovka Astronomical Observatory of the Ural Federal University(Russia) and the Three College Observatory of the University of North Carolina at Greensboro(USA) as well as archival spectral data compiled since 1994. We report new data points in the radial velocity curve of the He I 5876 ?A line near the extremal values of the radial velocity.

Optical Spectroscopic Monitoring Observations of a Young Binary Z CMa

The results of optical spectroscopic monitoring observations of a young binary system, Z CMa, are presented in this study. Z CMa consists of a Herbig Be star and an FU Orionis object, and it shows irregular light variation in the quiescent phase and exploding brightening in the outburst phase. Medium-resolution spectra were obtained on 21 nights between 2015 and 2019 using the Nayuta telescope in Japan. We also used five high-resolution spectra, obtained between 2008 and 2011, with the Keck Telescope. During the outburst phase, the intensity of the He I absorption line increased with an increase in the luminosity of the system. Because the He I absorption line is a characteristic feature of an early-type star, we considered that the outbursts were caused by the Herbig Be star. The equivalent widths of the [O I] line decreased with an increase in the luminosity of the system. We claim steady mass loss at the rate of The intensities of the Hα and Fe II emission lines did not change during the outbursts. However, the line intensities increased with an increase in the luminosity of the system in the quiescent phase. We consider that those lines are attributed to the FU Orionis object and the light variations in the quiescent phase were caused by the FU Orionis object.