Une nouvelle variable 3.1912 Coronae borealis
نویسندگان
چکیده
منابع مشابه
Fluorine in R Coronae Borealis Stars
Neutral fluorine (F i) lines are identified in the optical spectra of several RCoronae Borealis stars (RCBs) at maximum light. These lines provide the first measurement of the fluorine abundance in these stars. Fluorine is enriched in some RCBs by factors of 800 to 8000 relative to its likely initial abundance. The overabundances of fluorine are evidence for the synthesis of fluorine. These res...
متن کاملWinds in R Coronae Borealis Stars
We present new spectroscopic observations of the He I λ10830 line in R Coronae Borealis (RCB) stars which provide the first strong evidence that most, if not all, RCB stars have winds. It has long been suggested that when dust forms around an RCB star, radiation pressure accelerates the dust away from the star, dragging the gas along with it. The new spectra show that nine of the ten stars obse...
متن کاملUne nouvelle stratégie d'apprentissage Bayésienne
Les données D sont composées de deux sous-ensembles T et U qui correspondent respectivement aux données étiquetées et non-étiquetées, avec D = T ∪U . L’ensemble T contient des couples (x, y), où x ∈ R et y ∈ Y est une valeur discrète représentant la classe de l’exemple x. L’ensemble U contient des réels. Les notations suivantes sont adoptées : N , le nombre d’exemples observables (N = |D|) ; N ...
متن کاملThe MACHO Project LMC Variable Star Inventory : IV . New R Coronae Borealis
We report the discovery of two new R Coronae Borealis (RCB) stars in the Large Magellanic Cloud (LMC) using the MACHO project photometry database. The identiication of both stars has been connrmed spectroscopically. One is a cool RCB star (T eff 5000 K) characterized by very strong Swan bands of C 2 and violet bands of CN, and weak or absent Balmer lines, G-band and 12 C 13 C bands. The second ...
متن کاملH α variability of the recurrent nova T Coronae Borealis ⋆
We analyze Hα observations of the recurrent nova T CrB obtained during the last decade. For the first time the Hα emission profile is analyzed after subtraction of the red giant contribution. Based on our new radial velocity measurements of the Hα emission line we estimate the component masses of T CrB. It is found that the hot component is most likely a massive white dwarf. We estimate the inc...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Astronomische Nachrichten
سال: 1911
ISSN: 0004-6337,1521-3994
DOI: 10.1002/asna.19111902103