stellar mass loss oor Spaans
stellar mass loss
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Another feature of this class of stars is the stellar mass loss, in the case of W Aquilae is estimated at ~ 6993400000000000000♠4×10−7 solar masses per year.
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This issue was later resolved when new computer simulations, which included the effects of mass loss due to stellar winds, indicated a much younger age for globular clusters.
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Among the results are constraints set for the first time on the mass loss of red giant stars in open stellar clusters.
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Forming this type of star requires the red giant progenitor to eject almost its entire envelope via a mechanism that significantly amplifies the normal mass loss from stellar winds and it seems highly likely that the two planets discovered around this star may have triggered such a process.
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The star may also undergo mass loss by exceeding its Eddington luminosity, or through strong stellar winds, and some of this material may become gravitationally attracted to the neutron star.
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Although there is progress in understanding both stellar evolution and mass loss theoretically, observational details of, in particular, the last phase of the mass loss process have remained obscure.
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Rewinding stellar evolution: The last 400,000 years of mass loss from a star
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“If this is the case it suggests that binary systems may play a key role in stellar evolution by driving mass loss — the ultimate cosmic ‘diet plan’ for heavyweight stars, which shifts over 95% of their initial mass,” concludes Clark.
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To fully understand these observations, improved models of stellar winds will be needed, taking into account both the large-scale emission structures and the highly fragmented wind, in order to understand how they affect mass-loss in stellar giants.
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They are cool, red giants with large mass loss in the form of strong stellar winds, and are typically long-period variables.
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They are cool, red giants with large mass loss in the form of strong stellar winds, and are typically long-period variables.
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“Such huge mass losses before the explosion present great challenges to current theories of stellar evolution.”
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Stellar rotation affects the massive stellar evolution due to the rotationally induced mixing processes, the increase of mass loss rates, etc.
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Generally, the values agree fairly well, so that in principle one should be able to study mass loss as a function of stellar parameters, in particular of location on the Hertzsprung-Russell (HR) diagram.
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Our sample comprised post-AGB stars and young planetary nebulae (PNe), whose mass-loss processes and circumstellar structures resemble those of young stellar objects(YSOs), where methanol masers are detected.
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Sandin says that "In comparison to other methods which measure mass loss rates, our estimates are made directly on the gas component of the stellar wind."
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The stellar atmosphere modelling process is complicated by the severe conditions of NLTE, sphericity and mass loss, which effect is to couple the radiative transfer, statistical equilibrium and hydrodynamic equations in a spherical geometry.
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Although many stellar parameters can be obtained from the different spectral ranges, the UV is necessary to derive the terminal wind velocities and the optical or IR, for temperatures, gravities and mass-loss rates.
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They calculated new stellar evolution models including the effects of rotation and magnetic pairs under different assumptions. The objective was to test whether a single star could sustain the rotation speed necessary to generate a bipolar planetary nebula (PN), when high rates of mass loss are considered.
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19 sinne gevind in 10 ms. Hulle kom uit baie bronne en word nie nagegaan nie.