'Mass loss rate' presentation slideshows

X-ray Emission from O Stars

859 views • 69 slides

Lecture 8 Semiconvection, Mass Loss, and Rotation

Lecture 8 Semiconvection, Mass Loss, and Rotation. The three greatest uncertainties in modeling the presupernova evolution of single massive stars are: Convection and convective boundaries (undershoot, overshoot, semiconvection, late stages) Rotation

819 views • 68 slides

MESURES de DEGAZAGE G.Vandoni , CERN

MESURES de DEGAZAGE G.Vandoni , CERN. Definitions, Units Some theory and phenomenology with some tentative explanation Methods of measurement: Throughput conductance modulation two path Pressure rate-of-rise (accumulation) Coupling throughput and accumulation Total mass loss

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Cosmic Jets

598 views • 40 slides

X-ray Emission from O Stars

481 views • 37 slides

The synthesis of 26 Al and 60 Fe in massive stars and their current abundances in our Galaxy

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INAF, Osservatorio Astronomico di Roma

Radio-ejection in an interacting binary MSP in a Globular Cluster. F. D'Antona. INAF, Osservatorio Astronomico di Roma. XI Advanced School of Astrophysics, Brazil, 1-6 September 2002. The first MSP in an interacting binary: J1740-5340. and in a globular cluster!.

513 views • 31 slides

Stellar Winds and Mass Loss

Stellar Winds and Mass Loss. Brian Baptista. Summary. Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the ISM Effects on stellar evolution. Some History. Nova like objects are discovered Diagnostics of mass laws are generated for hot stars

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GRAPHITE SUBLIMATION TESTS with Inert Gas Mitigation

GRAPHITE SUBLIMATION TESTS with Inert Gas Mitigation. C. C. Tsai, T. A. Gabriel, J. R. Haines, and D. A. Rasmussen Oak Ridge National Laboratory 2 nd International High Power Targetry Workshop October 10 , 2005. ACKNOWLEDGEMENT. Thanks to :

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Stellar Structure and evolution

Stellar Structure and evolution. Lecture 11: Evolution of massive stars. Learning Outcomes. The student will learn the following concepts Evolution of a high mass star - burning stages and lifetimes The detailed model predictions and a schematic overview

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Crushing of interstellar gas clouds Part I - Thermal Conduction and Radiative Losses -

Heat Flux:. Equations:. *Cowie & Mckee 1977. Cloud Mass Fraction:. choose phi = 0.3 implies that no thermal precursor develops during the shock propagation, which is consistent with the fact that no precursor is observed in young and middle aged SNRs. Crushing of interstellar gas clouds

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Takaya Nozawa (IPMU, Univ. of Tokyo) Masaomi Tanaka, Keiichi Maeda (IPMU)

2010/12/16. Properties of interstellar and circumstellar dust as probed by mid-IR spectroscopy of supernova remnants ( 超新星残骸の中間赤外分光から探る星間・星周ダスト ). Takaya Nozawa (IPMU, Univ. of Tokyo) Masaomi Tanaka, Keiichi Maeda (IPMU) Itsuki Sakon (Univ. of Tokyo).

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Mass loss from stars and galaxies: impact on evolution

Mass loss from stars and galaxies: impact on evolution. Tiit Nugis (Tartu Observatory) February 27, 2007. Mass loss from stars. Mass loss = mass lost by stellar wind (steady outflow of the matter from the surface) or by shell ejections.

326 views • 11 slides