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Distinguishing post-AGB impostors in a sample of pre-main sequence stars
(EDP SCIENCES S A, 2011)
Context. A sample of 27 sources, cataloged as pre-main sequence stars by the Pico dos Dias Survey (PDS), is analyzed to investigate a possible contamination by post-AGB stars. The far-infrared excess due to dust present ...
Kinematic distances of pre-main-sequence stars in the Lupus star-forming region
(International Astronomical UnionBeijing, 2012)
To reliably determine the main physical parameters (masses and ages) of young stars, we must know their distances. While the average distance to nearby star-forming regions (<300 pc) is often known, the distances to ...
Kinematic distances of pre-main-sequence stars in the Lupus star-forming region
(International Astronomical UnionBeijing, 2012)
To reliably determine the main physical parameters (masses and ages) of young stars, we must know their distances. While the average distance to nearby star-forming regions (<300 pc) is often known, the distances to ...
A probable pre-main sequence chemically peculiar star in the open cluster Stock 16
(Oxford University Press, 2014-07)
We used the Ultraviolet and Visual Echelle Spectrograph of the ESO-Very Large Telescope to obtain a high resolution and high signal-to-noise ratio spectrum of Stock 16-12, an early-type star which previous Δa photometric ...
Pre-main-sequence stars in the Lagoon Nebula (M8)
(Oxford University Press, 2007-02)
We report the discovery of new pre-main-sequence (PMS) stars in the Lagoon Nebula (M8) at a distance of 1.25 kpc, based on intermediate-resolution spectra obtained with the Boiler & Chivens spectrograph at the 6.5-m Magellan ...
On be star candidates and possible blue pre-main sequence objects in the small magellanic cloud
(SPRINGER SCIENCE, 2002)
Detection of a giant flare displaying quasi-periodic pulsations from a pre-main-sequence M star by the Next Generation Transit Survey
(Oxford University Press, 2019)
We present the detection of an energetic flare on the pre-main-sequence M3 star NGTS J121939.5–355557, which we estimate to be only 2 Myr old. The flare had an energy of 3.2 ±0 0 4 3 ×1036 erg and a fractional amplitude ...