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STANDARD 4a
STANDARD 4a

Powerpoint
Powerpoint

... Until the temperature becomes very high (kT >> 1 MeV) The most abundant nuclei are those with large binding energy per nucleon and "natural" values of . For example, ...
The lifes of a star
The lifes of a star

... Recall that all atoms are made of a very dense and small nucleus which is positively charged and a bunch of electrons, which are negatively charged, and which surround the nucleus. At the center of the stars temperatures as very high (at least a few million degrees Celsius); pressures are also high ...
`Family of the Sun`
`Family of the Sun`

Revolving Planets Lesson Plan
Revolving Planets Lesson Plan

... Solar System Diagram Note: This diagram is not drawn to scale. It shows the order of the planets from the sun to Neptune, but does not aim to illustrate the distances between the planets. ...
Stellar Winds and Hydrodynamic Atmospheres
Stellar Winds and Hydrodynamic Atmospheres

... the implicit solution Eq. 8b for v(r) together with the conditions for the critical point Eq. 7a,b can be used to discuss topology of solution families ...
Radiation from Proxima Centauri
Radiation from Proxima Centauri

sources of hard and soft x-ray emission in solar flares: mhd simulation
sources of hard and soft x-ray emission in solar flares: mhd simulation

The Stellar Dynamo - Academic Program Pages
The Stellar Dynamo - Academic Program Pages

... of measuring the magnetic activity of roughly 100 so-called main-sequence stars—those that, like the sun, are burning hydrogen. (When the hydrogen runs out, a star expands into a red giant.) Most of these stars show obvious signs of magnetic activity, by way of variations in their violet calcium emi ...
The Stellar Dynamo - Department of Atmospheric Sciences
The Stellar Dynamo - Department of Atmospheric Sciences

... of measuring the magnetic activity of roughly 100 so-called main-sequence stars—those that, like the sun, are burning hydrogen. (When the hydrogen runs out, a star expands into a red giant.) Most of these stars show obvious signs of magnetic activity, by way of variations in their violet calcium emi ...
English - Cosmos
English - Cosmos

STARMASTER Planetarium Projector
STARMASTER Planetarium Projector

Chapter 22 - Heat Transfer p.430 Discover activity If several objects
Chapter 22 - Heat Transfer p.430 Discover activity If several objects

... terrestrial radiation. Over long averages, the amount of heat in the form of terrestrial radiation leaving the earth balances the solar radiation coming in, so the temperature remains stable and supports life. ”The near unanimous view of climate scientists is that human activity is a main driver of ...
Commentary on the Liquid Metallic Hydrogen Model of the Sun
Commentary on the Liquid Metallic Hydrogen Model of the Sun

Name
Name

... 2) A body takes 13 years to make one orbit around the Sun. What is the body’s semimajor axis? A) 4.3 AU B) 5.5 AU C) 2.9 AU D) 3.1 AU E) 4.6 AU 3) Who used Tycho Brahe’s data to derive his laws of planetary motion? A) Isaac Newton B) Galileo Galilei. C) Nicolas Copernicus. D) Aristotle E) Johannes K ...
Winds
Winds

Name
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30.4 Gravitational collapse & early protostellar evolution I (HB)
30.4 Gravitational collapse & early protostellar evolution I (HB)

... where collisonal dissociation of H2 starts. --> Temperature increase less steep - However, thermal energy per molecule at 2000K ~ 0.74eV compared to dissociation energy of H2 of ~ 4.48eV --> Even modest increase of dissociated H2 absorbs most of the gravitational energy from the collapse --> margina ...
Hertzsprung-Russell Diagram, Flux, Luminosity, Magnitude—10 Oct Outline •
Hertzsprung-Russell Diagram, Flux, Luminosity, Magnitude—10 Oct Outline •

... Is it flux or luminosity? • The color of my cat is a property of my cat. It does not  change with distance. I see the same color whether my  cat is 1’ or 10’ from me. 1. S1: The flux of a star does not change with distance.  S2: The luminosity does not change with distance. A. B. C. D. ...
Astro 204: Practice Questions Some of these questions are a bit
Astro 204: Practice Questions Some of these questions are a bit

1 - Università degli Studi dell`Insubria
1 - Università degli Studi dell`Insubria

... >H in the hard stage is proportional to a -/2 >K is typically positive, but the eccentricity evoution of the binary is modest >MBHB-star interactions flatten the stellar distribution >Interacting stars typically corotate with the MBHB >A mass of the order of 0.7M is ejected from the bulge on nearly ...
ISP205-2 Visions of the Universe The Big Questions
ISP205-2 Visions of the Universe The Big Questions

... The Birth of Science (for Thurs) 1. Arrange in order of increasing distance. a. Orion nebula, Jupiter, center of Milky Way, Andromeda galaxy b. Jupiter, Orion nebula, center of Milky Way, Andromeda galaxy c. Center of Milky Way, Orion nebula, Jupiter, Andromeda galaxy d. Jupiter, Center of Milky Way ...
slides ppt
slides ppt

... - correlated in time and direction with GRB • central engine also emits GW (compact object, relativistic motion) - scenarios to get BH+accretion disk : NS-NS, NS-BH mergers, failed SN - ‘canonical’ GW sources (inspiral  merger, collapse) - LIGO-Virgo only sensitive to 30 Mpc, advanced LIGO-Virgo to ...
PowerPoint - Chandra X
PowerPoint - Chandra X

... The H-alpha and X-ray data show evidence for star formation in the tails – the first unambiguous evidence that star formation can occur in gas stripped from galaxies. ...
Literature: The rotation of the Sun
Literature: The rotation of the Sun

... differentially and thus is not solid. This discovery helped revolutionize ideas about the nature of the Sun almost as effectively as the spectrum analysis that was going on in the same decade. More recently, astronomers have begun to suspect that this differential rotation of the Sun's outer layers ...
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Standard solar model

The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma). This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined. The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System. The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium. All heavier elements, called metals in astronomy, account for less than 2 percent of the mass. The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to ""fit"" the observed Sun.
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