Pre-Main-Sequence Stars
Magnetic fields and X ray emission in pre main sequence stars
... files of Zeeman sensitive spectral lines to constrain the distribution of field over the surface. However, since unpolarised line profiles yield no information about the orientation of the surface field, the MSI ...
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Submillimeter lines from circumstellar disks around pre-main sequence stars
... Circumstellar disks play an essential role in the under- standing of the formation of planetary systems such as our own (see Beckwith 1999; Beckwith & Sargent 1996 for recent reviews). These protoplanetary disks ...
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On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars
... with spectral types F and earlier more similar between them in the Balmer region than for later spectral types. Fig. 2 (top-right panel) illustrates the case; the photospheric U–B colour characterizing the Balmer region ...
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The Keele-Exeter young cluster survey - I. Low-mass pre-main-sequence stars in NGC 2169
... with stars at spectral type ≃ M2 and widening with age to encompass spectral types either side (see Jeffries ...convective stars reach a temperature sufficient to burn ...
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1-10 Myr-old Low Mass Stars and Brown Dwarfs in Nearby Star Forming Regions
... solar-type pre-main sequence stars may cause differences in the evolution of accretion, disk composition and grain ...mass stars to form planetary ...200 stars ranging from ∼ 20 ...
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Magnetic fields in O-, B- and A-type stars on the main sequence
... in pre-main sequence stars, hotter main-sequence stars, and more evolved ...of stars, for instance, in bright main-sequence A-type stars with ...
5
Mid IR spectra of pre main sequence Herbig stars : an explanation for the non detections of water lines
... Fig. 7. Herbig parameter space for the water line blend at 15.17 μm. In the plot the data points (all upper limits, in grey) are from Pontoppidan et al. (2010a). All the fluxes are scaled to 140 pc. The shaded yellow ...
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Magnetic fields and differential rotation on the pre-main sequence - III. The early-G star HD 106506
... nearby stars within the field of ...comparison stars within the same field of view, are ...standard stars in Graham’s E-regions (Graham ...the stars, including HD ...standard stars and ...
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Pre-main-sequence isochrones - I. The Pleiades benchmark
... MS stars, used their observed SDSS colours to establish their effective temperatures and then folded model at- mospheres of the appropriate temperature through our estimated system responses to find their ...
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On chromospheric variations modeling for main sequence stars of G and K spectral classes
... fields on the Sun and Sun-like stars emit Ca II H and K more intensely than areas with less magnetic field pre- sent. So the contrast of Active Regions (AR) emission (where the local magnetic fields are ...
5
Koenig, Brigitte (2003): Flare stars in the solar vicinity: A search for young stars. Dissertation, LMU München: Fakultät für Physik
... young stars in the solar vicinity and in an evolutionary stage between the classical T Tauri phase with a disk and the zero-age main sequence can be provided by the catalog of flare stars and ...
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The blue supergiant MN18 and its bipolar circumstellar nebula
... massive stars form their circumstellar nebu- ...Wolf–Rayet stars could exist until their central stars explode as ...these stars might be the immediate precursors of supernovae ...
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ZZ Cyg – FUNDAMENTAL PARAMETERS
... The WD output fundamental parameters and errors are listed in Table 5 and – for comparison – the corresponding values of zero age main sequence stars (Cox, 2000). Most of the errors are output or ...
6
Archaeoastronomical Study of the Main Pyramids of Giza, Egypt: Possible Correlations with the Stars?
... More pre- cisely the straight line connecting the south-eastern corners of the two extreme pyramids (those of Menkaure and Khufu) passes about 12 m away from the corresponding corner of the central (Khafre) ...
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Eclipsing white dwarf binaries
... Recent years have seen an explosion in the number of eclipsing binaries containing white dwarfs. In the last few years the number of systems has increased from 7 to over 40, thanks mainly to large surveys such as the ...
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Seismic signatures of stellar magnetic activity — what can we expect from TESS?
... of stars observed by Kepler (Borucki et ...24 stars in their sample showed significant and systematic frequency shifts in time, while Santos et ...these stars tend to be more active and consequently ...
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Review article Onbig Bangnucleosynthesis and formation of elements in stars
... Thus in this process, 4 protons fuse to form one He-4 nucleus but energy release is more than that in the proton-proton chain, so larger main sequence stars are brighter than smaller ones. ii) ...
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Star Notes.ppt
... • Extremely large stars (>20x solar masses in main sequence). – Red Supergiant Core explodes in supernova – Planetary nebula forms[r] ...
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The Problem of the Existence of Planetary Systems Similar to the Solar System
... k = T (18) For any couple of gaseous stars which can be compared between themselves [5]. Consequently, from rela- tionship (17) the following numerical equation for the calculation of β parameter for any gaseous ...
7
What CoRoT tells us about δ Scuti stars - Existence of a regular pattern and seismic indices to characterize stars
... of stars confirm these results, but in addition, we show on a large set of objects that these regularties are due to a regular pattern of con- secutive peaks which is compatible with patterns expected for ...
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