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Timescale of mass accretion in pre-main-sequence stars [PDF]
Astronomy and Astrophysics, 2010 We present initial result of a large spectroscopic survey aimed at measuring the timescale of mass accretion in young, pre-main-sequence stars in the spectral type range K0 - M5. Using multi-object spectroscopy with VIMOS at the VLT we identified the fraction of accreting stars in a number of young stellar clusters and associations of ages between 1 ...
Davide Fedele +2 more
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Infrared companions to pre-main sequence stars
Astrophysics and Space Science, 1988We report 1.2, 1.6, 2.2 and 3.6 μm slit scan observations of the young low-luminosity stars Elias 22 (also known as GSS 31) in the Rho Ophiuchus dark cloud and Glass I in the Chamaeleon dark cloud. We discovered an infrared companion to Elias 22 at a projected separation of 2.0 arcsec (320 AU) and an optical/infrared companion to Glass I at a projected
H. Zinnecker +4 more
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1987
The IUE satellite has inaugurated a new era in the study of pre-main sequence (PMS) objects. IUE observations have revealed not just a new wavelength range but also a new temperature regime embracing physical phenomena that could not be studied before.
Catherine L. Imhoff, I. Appenzeller
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The IUE satellite has inaugurated a new era in the study of pre-main sequence (PMS) objects. IUE observations have revealed not just a new wavelength range but also a new temperature regime embracing physical phenomena that could not be studied before.
Catherine L. Imhoff, I. Appenzeller
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Pre-Main-Sequence Binary Stars
Annual Review of Astronomy and Astrophysics, 1994The observational study of pre-main-sequence (PMS) binary stars is in many ways a very young field; most PMS binaries known today were discovered in the past decade. Nonetheless, T Tauri stars have been under study for more than a half century, and the serendipitous discovery of visual pairs has always been a by-product of their observation (e.g. Joy &
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2007
Herbig Ae/Be stars are the early-type pre-main sequence stars. Normally they are simply abbreviated as HES (Herbig emission-line stars) or HAEBE (Herbig Ae Be stars). (1960) originally defined HES by the following characteristics: (i) The spectral type is A or earlier, with emission lines. (ii) The star lies in an obscured region.
Tomokazu Kogure, Kam-Ching Leung
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Herbig Ae/Be stars are the early-type pre-main sequence stars. Normally they are simply abbreviated as HES (Herbig emission-line stars) or HAEBE (Herbig Ae Be stars). (1960) originally defined HES by the following characteristics: (i) The spectral type is A or earlier, with emission lines. (ii) The star lies in an obscured region.
Tomokazu Kogure, Kam-Ching Leung
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Revisiting the pre-main-sequence evolution of stars
Astronomy and Astrophysics, 2018 Aims. We want to investigate how planet formation is imprinted on stellar surface composition using up-to-date stellar evolution models.Methods. We simulate the evolution of pre-main-sequence stars as a function of the efficiency of heat injection during accretion, the deuterium mass fraction, and the stellar mass, M⋆.
Masanobu Kunitomo +2 more
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δ Scuti Pulsations in Pre-Main Sequence Stars
Astrophysics and Space Science, 2003Intermediate mass pre-main sequence stars (1.5 to 5 M ⊙) cross the instability strip on their way to the main sequence. They are therefore expected to be pulsating in a similar way as the δ Scuti stars. In this review, I present the status of observational studies of pulsations in these stars, and comment on prospects for future investigations of these
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Pre-Main-Sequence Stages of Stars
Publications of the Astronomical Society of Japan, 1965Abstract Evolutionary model sequences of gravitationally contracting stars were calculated for masses, 0.4, 0.6, 1.0, 1.5, 2.0 and 3.0 M⊙, by using the surface condition based on the conventional mixing length theory of convection and assuming the contraction to be homologous. The mixing length was assumed to be equal to 1-pressure scale
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An emission sequence in pre-main-sequence flare stars
Monthly Notices of the Royal Astronomical Society, 1991Optical spectra of quiescent pre-main-sequence flare stars in Orion are presented. The spectra cover ∼3600-4600 A at ∼3 A resolution, and were taken using an optical fibre fed spectrograph. The spectra reveal that most of the stars have Ca II H and K and the Balmer lines in emission, and approximate surface fluxes for these lines are deduced, along ...
B. D. Carter, B. J. O'Mara
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The Evolution of Pre-Main-Sequence Stars
1999The location of optically visible Pre-Main-Sequence (PMS) stars in the H-R diagram combined with the use of theoretical evolutionary tracks have played a central role in stellar evolution studies since the initial work of Hayashi, Cameron and Iben in the early ′60s.
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