Emission line stars: Be
The Gaia satellite: a tool for Emission Line Stars and Hot Stars
... will be launched in ...to be 5 ...all stars down to V magnitude 20 with an accuracy 200 times better than ...GK stars). This last one will provide spectra for stars till V magnitude ...
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Spectro-interferometric observations of a sample of Be stars Setting limits to the geometry and kinematics of stable Be disks
... bright Be stars: α Col, κ CMa, ω Car, p Car, δ Cen, µ Cen, α Ara, and o ...Brγ emission line to study the kinematics within the circumstellar ...the line and the nearby continuum for ...
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VLTI/MIDI observations of 7 classical Be stars
... – Stars: emission-line, Be – Stars: winds, outflows, disks – Stars: individual (p Car, ζ Tau, κ CMa, α Col, δ Cen, β CMi, α Ara) – Stars: circumstellar matter ...Classical ...
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Be stars in open clusters in the Small Magellanic Cloud.
... the Be phenomenon accross the Large and Small Magellanic ...the Be phenomenon with the ...the Emission line ...the stars and give answers about the origin of the Be ...
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Coronagraphic imaging of three weak-line T Tauri stars: evidence of planetary formation around PDS 70
... can be explained either by thermal instabilities or by the dynamical effects of the brown dwarf com- ...thermal emission in the far infrared can only be explained by the presence of a young cold ...
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On the nature of early-type emission line objects in NGC6611
... EARLY-TYPE EMISSION LINE OBJECTS IN NGC6611 ...of emission line stars in the young open cluster NGC6611 is still the object of ...of emission line stars is highly ...
5
The [CII] 158 μm line emission in high-redshift galaxies
... [OIII] line, orig- inating from di ffuse and highly ionized regions near young O stars, is a promising line (Inoue et ...[CII] line, predominantly originating from PDRs at high redshift ...
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Massive Be and Oe stars at low metallicity and long gamma ray bursts
... of Be stars at low metallicity Maeder et ...of Be stars by open clusters seems to increase with the decrease of the environment ...of stars and open clus- ters used is relatively small ...
7
Evolution and appearance of Be stars in SMC clusters
... Keywords. stars: emission-line, Be, stars: fundamental parameters, stars: statistics, stars: early- type, stars: evolution, surveys, galaxies: star clusters, ...
5
THE LONG-TERM H$\alpha$ EMISSION LINE VARIATION IN $\alpha$~Eri
... of Be stars are their phase B⇀ ↽Be⇀ ↽Be- shell transitions evidenced by the Balmer line emission intensity ...can be ought either to variations of the physical structure ...
3
ZAMS rotational velocities of Be/Oe stars and LGRBs progenitors in the Magellanic Clouds.
... B-type stars are expected to be higher in low metallicity (LMC/SMC) than in high metallicity (MW) ...and Be stars, which form, at the moment, the largest observed sample of these kind of ...
5
Three discoveries of γ Cas analogues from dedicated XMM-Newton observations of Be stars
... could be expected from a PMS ...to be significantly variable and the spectra of HD 44458 and HD 45995 clearly show the presence of the iron complex ...to be ob- served with eROSITA (PI: ...disk ...
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New atmosphere models for massive stars: line-blanketing effects and wind properties of O stars
... extended, line-blanketed models was made by Abbott & Hummer (1985) who improved the non-LTE models of Mihalas (1972) by adding a wind component above the photo- sphere in a so-called core-halo approach in ...
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A slitless spectroscopic survey for Halpha emission-line objects in SMC clusters
... 26 Be stars, among them 6 candidates, within a radius of ...17 stars in common, of which Album rejected 8 highly blended ...9/17 stars is consistent with the estimated general extraction ...
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On the behaviour of B and Be stars at low metallicity.
... between stars with and without line emission at ...distinguish emission-line stars (ELS) from other objects, we created the ALBUM package in ...
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Be stars: one ring to rule them all ?
... al.: Be stars: one ring to rule them all ? 5 the fading of emission characteristics would correspond either to a cavity formation according to the ring scenario or to a disc dissipation carried by a ...
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Variability of B and Be stars in the LMC/SMC: binaries and pulsations.
... and Be stars observed in the Magellanic clouds with the VLT-FLAMES, we cross-matched the stars of our sample with the photometric database MACHO, which provides for each star an 8 years ...these ...
5
Long Baseline Interferometry of Be Stars
... tral line) science channel at wavelength λ s . This can be performed by means of cross-correlation of a broad continuum channel with a series of narrow channels across the emission line as ...
9
Review about populations of Be stars: stellar evolution of extreme stars
... of Be stars is the veiling effect due to the circumstellar disk that affects the continuum level and thus the lines ...He4471 emission-line EW ...
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Be stars and binaries in the field of the SMC open cluster NGC330 with VLT-FLAMES
... of Be stars in the SMC. The first column gives the name of the Be star in the EIS catalogue or following our catalogue if the star is not found in the EIS ...present emission components, ...
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