Results 51 to 60 of about 226,792 (352)

Photometric Determination of the Mass Accretion Rates of Pre-main-sequence Stars. V. Recent Star Formation in the 30 Dor Nebula [PDF]

, 2017
We report on the properties of the low-mass stars that recently formed in the central of 30 Dor, including the R136 cluster. Using the photometric catalog of De Marchi et al., based on observations with the Hubble Space Telescope, and the most recent ...
G. Marchi, N. Panagia, G. Beccari
semanticscholar   +1 more source

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, D. Gouliermis, R. Klessen, E. Grebel, E. Sabbi, Jay Anderson, D. Lennon, M. Cignoni, G. Marchi, Linda J. Smith, M. Tosi, Roeland P. van der Marel Institut fur Theoretische Astrophysik, Zentrum fur Astronomie der Universitat Heidelberg, Interdisciplinary Center for Scientific Computing, U. Heidelberg, M. F. Astronomy, A. Rechen-Institut, Space Telescope Science Institute, Esa European Space Astronomy Center, D. Physics, University of Pisa, European Space Research, T. Centre, E. S. Agency, I. Bologna   +24 more
semanticscholar   +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

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, T. Guillot, S. Ida, T. Takeuchi   +3 more
semanticscholar   +1 more source

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., Dupret, Marc-Antoine, Garrido, Rafael, Gabriel, M., Scuflaire, Richard   +4 more
openaire   +2 more sources

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, Mario Gennaro, Nicola Da Rio, Giovanni Maria Strampelli, Leonardo Ubeda, Elena Sabbi, Dana Koeppe, Jonathan C. Tan, David R. Soderblom   +8 more
doaj   +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, David B. Guenther, Konstanze Zwintz   +2 more
openaire   +3 more sources

Are pre-main-sequence stars older than we thought? [PDF]

, 2009
We fit the colour-magnitude diagrams of stars between the zero-age main-sequence and terminal-age main sequence in young clusters and associations. The ages we derive are a factor 1.5 to 2 longer than the commonly used ages for these regions, which are ...
Alibert, Ayliffe, Bessell, Bessell, Blaauw, Brown, Brun, Claria, Dodson-Robinson, Eggen, Fernie, Girardi, Haisch, Hertzsprung, Hillenbrand, Horch, Hubickyj, Høg, Høg, Jeffries, Jeffries, Jeffries, Johnson, Johnson, Joshi, Lejeune, Maeder, Maeder, Mayne, Mayne, Meynet, Meynet, Mordasini, Murdin, Naylor, Pollack, Ramírez, Schaller, Sherry, Stauffer, Stauffer, ten Brummelaar, Tim Naylor, Walker, Walker, Walker   +45 more
core   +2 more sources

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, R. Jackson, E. Franciosini, S. Randich, D. Barrado, A. Frasca, A. Klutsch, A. Lanzafame, L. Prisinzano, G. Sacco, G. Gilmore, A. Vallenari, E. Alfaro, Sergey E. Koposov, E. Pancino, A. Bayo, A. Casey, M. Costado, F. Damiani, A. Hourihane, J. Lewis, P. Jofré, L. Magrini, L. Monaco, L. Morbidelli, C. Worley, S. Zaggia, T. Zwitter   +27 more
semanticscholar   +1 more source

The Effect of Pre–Main‐Sequence Stars on Star Cluster Dynamics [PDF]

The Astrophysical Journal, 2006
We investigate the effects of the addition of pre-main sequence evolution to star cluster simulations. We allowed stars to follow pre-main sequence tracks that begin at the deuterium burning birthline and end at the zero age main sequence. We compared our simulations to ones in which the stars began their lives at the zero age main sequence, and also ...
Wiersma, R., Sills, A., Portegies Zwart, S.F.   +2 more
openaire   +4 more sources