Results 51 to 60 of about 451,529 (372)
Hubble Tarantula Treasury Project - VI. Identification of pre-main-sequence stars using machine-learning techniques [PDF]
, 2018 The Hubble Tarantula Treasury Project (HTTP) has provided an unprecedented photometric coverage of the entire star-burst region of 30 Doradus down to the half Solar mass limit.
Victor F. Ksoll +24 more
semanticscholar +1 more source
Revisiting the pre-main-sequence evolution of stars [PDF]
Astronomy & Astrophysics, 2017 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 ...
M. Kunitomo +3 more
semanticscholar +1 more source
An HST Study of the Substellar Population of NGC 2024
The Astrophysical Journal, 2023 We performed an HST/WFC3-IR imaging survey of the young stellar cluster NGC 2024 in three filters probing the 1.4 μ m H _2 O absorption feature, characteristic of the population of low-mass and substellar-mass objects down to a few Jupiter masses.
Massimo Robberto +8 more
doaj +1 more source
Accretion onto Pre-Main-Sequence Stars
, 2016 Accretion through circumstellar disks plays an important role in star formation and in establishing the properties of the regions in which planets form and migrate. The mechanisms by which protostellar and protoplanetary disks accrete onto low-mass stars
L. Hartmann, G. Herczeg, N. Calvet
semanticscholar +1 more source
Nonradial Oscillations on a Pre–Main‐Sequence Star [PDF]
The Astrophysical Journal, 2007 We show that the modes observed on the pulsating pre-main-sequence (PMS) star NGC 6383 170 can be interpreted as a combination of radial and nonradial p-modes. Using a dense grid of PMS models and oscillation spectra, we have identified models that match the observed oscillation spectrum within 1 σ of the frequency uncertainties and are consistent with
W. W. Weiss +2 more
openaire +3 more sources
Instability strip for pre-main-sequence stars [PDF]
Communications in Asteroseismology, 2007 We apply the Time Dependent Convection (TDC) treatment presented in Grigahcene et al. (2005) to the study of Pre-main sequence pulsating stars. The stabilization of the p-modes at the red edge of the Instability Strip (IS) is obtained by our models. The theoretical IS obtained with Mixing Length (ML) parameter α =1.8 is compared to observations and a ...
Grigahcène, A. +4 more
openaire +2 more sources
Magnetic fields and differential rotation on the pre-main sequence [PDF]
, 2009 Maps of magnetic field topologies of rapidly rotating stars obtained over the last decade or so have provided unique insight into the operation of stellar dynamos. However, for solar-type stars many of the targets imaged to date have been lower-mass zero-
Carter, Bradley D. +2 more
core +1 more source
The Gaia-ESO Survey: lithium depletion in the Gamma Velorum cluster and inflated radii in low-mass pre-main-sequence stars [PDF]
Monthly notices of the Royal Astronomical Society, 2016 RDJ and RJJ acknowledge support from the UK Science and Technology Facilities Council (STFC). Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under programme ID 188.B ...
R. Jeffries +27 more
semanticscholar +1 more source
Magnetic Activity–Rotation–Age–Mass Relations in Late-pre-main-sequence Stars
The Astrophysical Journal, 2023 We study the four-dimensional relationships between magnetic activity, rotation, mass, and age for solar-type stars in the age range 5–25 Myr. This is the late-pre-main-sequence (l-PMS) evolutionary phase when rapid changes in a star's interior may lead ...
Konstantin V. Getman +2 more
doaj +1 more source
A CONSTRAINT ON THE FORMATION TIMESCALE OF THE YOUNG OPEN CLUSTER NGC 2264: LITHIUM ABUNDANCE OF PRE-MAIN SEQUENCE STARS [PDF]
, 2016 The timescale of cluster formation is an essential parameter in order to understand the formation process of star clusters. Pre-main sequence (PMS) stars in nearby young open clusters reveal a large spread in brightness.
B. Lim +5 more
semanticscholar +1 more source