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Massive pre-main-sequence stars in M17 [PDF]
Proceedings of the International Astronomical Union, 2017 The formation process of massive stars is still poorly understood. Massive young stellar objects (mYSOs) are deeply embedded in their parental clouds; these objects are rare, and thus typically distant, and their reddened spectra usually preclude the ...
M. Ram'irez-Tannus +8 more
semanticscholar +9 more sources
IRAC Observations of Taurus Pre-Main-Sequence Stars [PDF]
The Astrophysical Journal, 2005 We present infrared photometry obtained with the IRAC camera on the Spitzer Space Telescope of a sample of 82 pre-main-sequence stars and brown dwarfs in the Taurus star-forming region. We find a clear separation in some IRAC color-color diagrams between
L. Hartmann +7 more
semanticscholar +6 more sources
X-Ray Superflares from Pre-main-sequence Stars: Flare Energetics and Frequency [PDF]
Astrophysical Journal, 2021 Solar-type stars exhibit their highest levels of magnetic activity during their early convective pre-main-sequence (PMS) phase of evolution. The most powerful PMS flares, superflares and megaflares, have peak X-ray luminosities of log(LX)=30.5–34.0 erg s−
Konstantin V. Getman, Eric D. Feigelson
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The ages of pre-main-sequence stars [PDF]
Monthly Notices of the Royal Astronomical Society, 1999 The position of pre-main-sequence or protostars in the Hertzsprung--Russell diagram is often used to determine their mass and age by comparison with pre-main-sequence evolution tracks. On the assumption that the stellar models are accurate, we demonstrate that, if the metallicity is known, the mass obtained is a good estimate.
Tout, Christopher A. +2 more
openaire +4 more sources
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS [PDF]
, 2013 We present an analysis of the intrinsic colors and temperatures of 5–30 Myr old pre-main-sequence (pre-MS) stars using the F0- through M9-type members of nearby, negligibly reddened groups: the η Cha cluster, the TW Hydra Association, the β Pic Moving ...
M. Pecaut, E. Mamajek
semanticscholar +3 more sources
Tracing early stellar evolution with asteroseismology: pre-main sequence stars in NGC 2264 [PDF]
EPJ Web of Conferences, 2015 Asteroseismology has been proven to be a successful tool to unravel details of the internal structure for different types of stars in various stages of their main sequence and post-main sequence evolution.
Zwintz Konstanze +4 more
doaj +4 more sources
Pre-Main-Sequence A-type stars [PDF]
Proceedings of the International Astronomical Union, 2004 Young A-type stars in the pre--main-sequence (PMS) evolutionary phase are particularly interesting objects since they cover the mass range (1.5-4 solar ma sses) which is most sensitive to the internal conditions inherited during the protostellar phase ...
Marcella Marconi, Francesco Palla
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Rotation and Activity of Pre–Main‐Sequence Stars [PDF]
The Astrophysical Journal, 2007 40 pages, 8 figures, ApJ, in ...
Scholz, Aleks +3 more
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Timescale of mass accretion in pre-main-sequence stars [PDF]
, 2009 We present the 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.
Davide Fedele +5 more
semanticscholar +3 more sources
The Instability Strip for Pre–main-sequence Stars [PDF]
The Astrophysical Journal, 1998 We investigate the pulsational properties of Pre--Main-Sequence (PMS) stars by means of linear and nonlinear calculations. The equilibrium models were taken from models evolved from the protostellar birthline to the ZAMS for masses in the range 1 to 4 solar masses.
Marconi, M., Palla, F.
openaire +5 more sources