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The Sun`s magnetic field
The Sun`s magnetic field

The Solar System
The Solar System

Neutrino Sources and Detectors
Neutrino Sources and Detectors

Stars with T eff
Stars with T eff

... • last generations of stellar models agree – almost all – within ≈ 0.003M • a fraction of the difference in McHe is due to the various initial He contents – but in the case of the Padua models… • the difference in Mbol(TRGB) is of the order of 0.15 mag when excluding the Padua models… ...
white dwarfs, neutron stars, black hole
white dwarfs, neutron stars, black hole

... It is now understood that all stars on the main sequence generate energy by the same mechanism, namely by fusing hydrogen into helium. The scattering of stars along the band of the main sequence is a consequence of their different initial masses. For main sequence stars, there is a simple relationsh ...
Part 2 - Stellar Evolution
Part 2 - Stellar Evolution

... • Fusion is much faster than PP-chain • C, N, O act as catalysts ...
PPT
PPT

... Need the distance D! Also need to know what fraction of the stellar surface radiates! The Magnificent Seven: seven soft X-ray sources with a ‘stellar’ spectrum and a distance estimate ...
What makes stars tick?
What makes stars tick?

Lecture11-ASTA01 - University of Toronto
Lecture11-ASTA01 - University of Toronto

DM in the Galaxy - University of Oxford
DM in the Galaxy - University of Oxford

... evidence for a ring 13
Meet Our Solar System
Meet Our Solar System

... Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, and Pluto 6. Cut each strip of blue construction paper into three pieces. Make two 9-cm pieces and one 10-cm piece. With a black marker, write the name of one planet lengthwise on each strip of paper. Use the longest pieces for the longe ...
ppt format
ppt format

... “see” at 10 microns we would “glow in the dark”!) In everyday life we see things by the light they reflect from hotter sources (Sun, light bulbs) rather than light they emit. ...
Unit 5 - Stars
Unit 5 - Stars

... For each helium atom created, place one bead next to it Continue this until all your Hydrogen supply is gone Write down how many Helium atoms there are Leave the 7 beads in the Helium quadrant. At this point 5 beads (energy) have been created in your Helium section. These are released in the form of ...
8-4 Asssessment 8-4.1 ______ (8-4.1) Which bodies are composed
8-4 Asssessment 8-4.1 ______ (8-4.1) Which bodies are composed

... 71. (8-4.10) The surface of Mars, the atmosphere of Jupiter, water spewing from the rings of Saturn, photographs of many of the other eight planets in the solar system: all valuable information collected by… a. manned space craft. b. satellite imaging. c. space probes. d. X-ray telescopes. ...
ppt - Wladimir Lyra
ppt - Wladimir Lyra

... The kinetic energy that was directed inwards is redirected outwards ...
8-4 Asssessment 4. The objects people refer to as shooting stars are
8-4 Asssessment 4. The objects people refer to as shooting stars are

... 71. (8-4.10) The surface of Mars, the atmosphere of Jupiter, water spewing from the rings of Saturn, photographs of many of the other eight planets in the solar system: all valuable information collected by… a. manned space craft. b. satellite imaging. c. space probes. d. X-ray telescopes. ...
Ay 102: Homework 5 (Blast waves, Supernova Remnant) S. R. Kulkarni
Ay 102: Homework 5 (Blast waves, Supernova Remnant) S. R. Kulkarni

... 1050 erg and mass of ejecta (predominantly heavy elements) could be as much as 0.1 M . Redo the calculations for phase 1 and phase 2. 3. Stellar Winds Consider a star with a strong stellar wind: Ṁ = 10−6 M yr−1 and terminal velocity, vw = 103 km s−1 embedded in a medium with density, n0 . As befo ...
Radiation vs. Gas Pressure, the Stellar Mass
Radiation vs. Gas Pressure, the Stellar Mass

... way possible, building in some ways on the basis developed last winter in Rich, Ken and my analyses of stellar structure within the “Eddington Standard Model” (ESM).1 Compared to those notes, the analysis here is quite rough and approximate, but hopefully it will help further clarify some key physic ...
Stars Part Two
Stars Part Two

... Helium Fusion: 1. When the core gets hot and dense enough, He begins to fuse: 4He + 4He = 8Be + γ 4He + 8Be = 12C + γ 2. The star contracts slightly and heats up, moving along the horizontal branch 3. Before the He is used up these reactions ...
Geochemistry & Lab
Geochemistry & Lab

Stellar Evolution Task
Stellar Evolution Task

... You will have noticed that some horizontal branch stars seemed to be above the normal region favoured by the others. These special stars are variable stars. Maybe you can spot them in the image of an old stellar cluster. These special stars are used to determine distance in our Galaxy. ...
The Story of Pulsational Pair-Instability SNe
The Story of Pulsational Pair-Instability SNe

Introduction to Astrophysics, Lecture 10
Introduction to Astrophysics, Lecture 10

... the star, and nuclear burning begins. This happens when the temperature reaches several million degrees. By now any planet formation should also have taken place. ...
Slides from Lecture19 - Department of Physics & Astronomy
Slides from Lecture19 - Department of Physics & Astronomy

... Real ‘All Sky’ Images of ...
Life Cycle of STARS
Life Cycle of STARS

... • Are stars BORN??? • Take a moment to think about our own Sun, and write down an idea about how it was formed using what we have learned so far. ...
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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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