'Radiative equilibrium' diaporamas de présentation

Metallicity Dependence of Winds from Red SuperGiants and Asymptotic Giant Branch Stars

Metallicity Dependence of Winds from Red SuperGiants and Asymptotic Giant Branch Stars. Jacco van Loon Keele University. Jacco van Loon Keele University. Dust wind structure. Radiative equilibrium + continuity equation:. Spectral Energy Distribution. Spectral Energy Distribution.

1.05k views • 91 slides

Radiative Transfer in the Atmosphere

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Rotation of Regulus

Rotation of Regulus. Age: a few hundred million years Mass: 3.5 solar masses Rotation Period: <1 day Equatorial Velocity: 200 km s -1 Axial tilt: 86 degrees from celestial north Gravity darkening: poles 15,000K equator 10,000K 5 times brighter at the poles.

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424 views • 42 slides

Modeling the Structure of Hot Star Disks

Modeling the Structure of Hot Star Disks. Jon E. Bjorkman Ritter Observatory. Systems with Disks. Infall + Rotation Young Stellar Objects (T Tauri, Herbig Ae/Be) Mass Transfer Binaries Active Galactic Nuclei (Black Hole Accretion Disks) Outflow + Rotation

611 views • 33 slides

Radiative Equilibrium

Radiative Equilibrium. Energy conservation. Radiative Equilibrium. Assumption : Energy conservation, i.e., no nuclear energy sources Counter-example: radioactive decay of Ni 56 ? Co 56 ? Fe 56 in supernova atmospheres Energy transfer predominantly by radiation Other possibilities:

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MET 61 Introduction to Meteorology - Lecture 8

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Ivan Hubeny University of Arizona

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The Atmosphere: Part 3: Unsaturated convection

The Atmosphere: Part 3: Unsaturated convection. Composition / Structure Radiative transfer Vertical and latitudinal heat transport Atmospheric circulation Climate modeling. Suggested further reading: Hartmann, Global Physical Climatology (Academic Press, 1994).

432 views • 23 slides

Radiative Forcing

Radiative Forcing. The balance between incoming solar radiation and heat radiation leaving the atmosphere. Key Findings. Extremely likely (> 95%) that humans have exerted a substantial warming influence on climate since 1750.

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Changes in Radiative Forcing

Changes in Radiative Forcing. Primary Source: IPCC WG-I Chapter 2 - Changes in Atmospheric Constituents and in Radiative Forcing. Key Findings. Extremely likely (> 95%) that humans have exerted a substantial warming influence on climate since 1750.

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NATS 101 Updates

NATS 101 Updates. Add your name to Class ListServe! First QUIZ on today Some textbooks at Park & University Book store 1st anniversary of Katrina this week Quick update on Ernesto & John. NATS 101. Lecture 4 Radiation. What is Temperature?. Microscopic View

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The Model Photosphere (Chapter 9)

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NATS 101 Lecture 5 Radiation

NATS 101 Lecture 5 Radiation. Radiation. Any object that has a temperature greater than 0 K, emits radiation. This radiation is in the form of electromagnetic waves, produced by the acceleration of electric charges.

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The Model Photosphere (Chapter 9)

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Energy Transport

Energy Transport. Formal solution of the transfer equation Radiative equilibrium The gray atmosphere Limb darkening. The Transfer Equation. Recall : for radiation passing through a gas, the change in I n is equal to: dI n = intensity emitted – intensity absorbed

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4.1 OPACITY

4.1 OPACITY.

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7.2.1 Equation of Phonon Radiative Transfer

7.2.1 Equation of Phonon Radiative Transfer. Dongwoo , Shin. Contents. Equation of Radiative Transfer (ERT) Equation of Phonon Radiative Transfer. Equation of Radiative Transfer.

336 views • 12 slides

9. Model Atmospheres

9. Model Atmospheres. Rutten: 7.1, 7.2 Assumptions Gas law, equation of state Hydrostatic equilibrium Temperature stratification Radiative equilibrium. Model Atmospheres. Problem: Construct a numerical model of the atmosphere to estimate

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Radiative Equilibrium

269 views • 7 slides