Massive stars
Identification of a population of X ray emitting massive stars in the galactic plane
... The radio spectrum of a single WR star with an optically thick stellar wind is thermal and has a spectral index of α ≈ +0.7 ± 0.1 (Dougherty & Williams 2000). If the wind is optically thin and has a radio spectral ...
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Prinz, Tobias (2013): Exploring the end states of massive stars using the X-ray emission of neutron stars and supernova remnants. Dissertation, LMU München: Fakultät für Physik
... of massive stars or the thermonuclear disruption of white dwarfs, are rare events, occurring on average every 50 years in the Galaxy (Keane and Kramer, ...guest stars by ancient Chinese astronomers ...
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HIPPARCOS photometry of 24 variable massive stars (alpha Cygni variables)
... These massive stars show without ex- ception photometric micro variations, also referred to as α Cyg–type variations, provided that they are evolved and massive enough ( > ∼ 25 M i /M ...
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Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies
... young massive stars is re- sponsible for creating H ii regions (Kennicutt 1998), correlations between di ff erent SN types and the Hα emission from their host galaxies can also be used to statistically ...
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The standard model of low-mass star formation applied to massive stars: a multi-wavelength picture of AFGL 2591
... that massive stars form as a scaled-up version of low-mass star formation, in this paper we aim to probe the circumstellar environment of the massive star-forming re- gion AFGL 2591 by combining ...
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The standard model of low-mass star formation applied to massive stars: multiwavelength modelling of IRAS 20126+4104
... whether massive stars form similarly to their low-mass counterparts, we have used the standard envelope plus disc geometry successfully applied to low-mass protostars to model the near-IR to submillimetre ...
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The origin of ejecta nebulae surrounding massive stars
... In recent years, largely due to increasing com putational power, stellar models have become very much more sophisticated. They are now able to broadly reproduce the observational characteristics and population statistics ...
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Light variations of massive stars (alpha Cyg variables). XV. The LMC supergiants R99 (LBV), R103, R123 (LBV) and R128
... of massive stars has led to the publication of a series of papers by the first author during the last 13 ...evolved massive stars are photometric micro variables also called α Cygni ...
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Fierlinger, Katharina M. (2014): Massive stars shaping the ISM: simulations and application to the Orion-Eridanus Superbubble. Dissertation, LMU München: Fakultät für Physik
... in stars and distributed throughout ...of stars. In this cycle, stars form in gas clouds, start nucleosynthesis, produce heavy elements and finally, when they have consumed their fuel for ...
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The role of massive stars in young starburst galaxies
... containing massive stars with masses > 100 ...from massive stars and su per novae ...the massive star ...O stars, early B supergiants and Wolf-Rayet stars which have ...
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Non-linear oscillations of massive stars
... More recently, Gurm [4], basing his computations on an exact stellar model of ten solar masses (§1.2)^ derived by numerical inte gration the first four modes of oscillation for an early main-sequence star. The case for ...
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Evolution and fate of very massive stars
... for stars with the same CO core found in various studies of VMS in the early Universe (Bond, Arnett & Carr 1984; Heger & Woosley 2002; Chatzopoulos & Wheeler 2012; Dessart et ...below, stars ...
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Non-radial oscillations and vibrational stability of massive stars initially composed of pure hydrogen
... In t he study of the vibrational stability of n on-radial oscillations of massiv e stars, we shall use the equilibrium models of stars composed of pure hydrogen constructed by Van der Bo[r] ...
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Hoffmann, Tadziu (2004): Synthetic spectra of massive stars as tool for the spectral analysis of stars and stellar clusters. Dissertation, LMU München: Fakultät für Physik
... In recent years there has been substantial progress in the mod- elling of expanding atmospheres of hot stars. It is now pos- sible to produce synthetic UV spectra of O stars that resem- ble the real, ...
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Reaction rate for carbon burning in massive stars
... Instead we note that the S factor appears to decline towards the lower energy region and exhibits a weak maximum around 3.5-4 MeV, a behavior similar to the hindrance phenomenon found te[r] ...
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Elements of Stars
... More massive stars end their lives due to the final collapse of their Fe-rich core. Once nuclear fusion pro- cesses have turned all the material in the core into Fe, neither fusion nor fission processes can ...
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On the Ultimate Fate of Massive Neutron Stars in an Ever Expanding Universe
... first stars must have been 100 to 10,000 solar masses and that they should have formed from primordial clouds made solely of hydrogen ...these massive stars must have collapsed directly into stellar ...
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Non-standard s-process in massive rotating stars - Yields of 10–150 M⊙ models at Z = 10E−3
... of stars with [Fe/H] < −3 are CEMP (with [C/Fe] > ...the stars showing clear overabundances of neutron-capture ...CEMP stars and normal metal-poor halo stars is likely due to the degree ...
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Massive main-sequence stars evolving at the Eddington limit
... all stars above ∼40 M reach the Eddington limit in their ...for massive stars in our ...of stars for which this limit comes down even ...rotating stars may lead to similar conditions in ...
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Hot stars observed by XMM-Newton. II. A survey of Oe and Be stars
... We examined each individual spectrum and fit it only if there were enough counts (or bins) to do so, which was the case for 51 stars. Table 3 provides the fitting results. Fitting was made within Xspec v12.9.1p ...
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