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Lecture 12: Age, Metalicity, and Observations Abundance
Lecture 12: Age, Metalicity, and Observations Abundance

File
File

... Larger, hotter main sequence stars, operating at higher core temperatures, can fuse hydrogen via the CNO cycle where carbon, nitrogen and oxygen act as catalysts in the reaction steps to produce helium. Process is cyclical Red-Giants (Post-main sequence) fuse heavier elements successively in their c ...
Lecture 21
Lecture 21

... cycle, a layer of stellar material loses support against the star’s gravity and falls inwards. • This inward motion tends to compress the layer, which heats up and becomes more opaque to radiation. • Since radiation diffuses more slowly through the layer (as a consequence of its increased opacity), ...
updated
updated

... state where the core temperature is too cool to fuse carbon. The core then collapses and heats in the same manner as occurred when core hydrogen was exhausted. ...
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... hydrodynamics are not invariant under a Galilean transformation. We therefore rephrase them using variables that are scaled to take into account the secular expansion of the gas. This gives equations that describe a spherically symmetric stellar wind but have almost the same form as the planar equat ...
The Chemical Composition of the Local Interstellar Dust
The Chemical Composition of the Local Interstellar Dust

SS_L2 - TCD Maths
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powerpoint file - QUB Astrophysics Research Centre
powerpoint file - QUB Astrophysics Research Centre

... hence much of the heat used to raise the temperature of the gas goes into ionisation and hence the specific heat of the gas at constant V is nearly the same as the specific heat at constant P , and ~1. In such a case, a star can have a cool outer convective layer. We will come back to the issues of ...
L4 - QUB Astrophysics Research Centre
L4 - QUB Astrophysics Research Centre

... hence much of the heat used to raise the temperature of the gas goes into ionisation and hence the specific heat of the gas at constant V is nearly the same as the specific heat at constant P , and ~1. In such a case, a star can have a cool outer convective layer. We will come back to the issues of ...
The Reason for the Seasons
The Reason for the Seasons

... explain the seasons! So far we only know why the hottest part of each planet is around the middle…the sunlight hits that part most directly. If that was all that happened, though, we WOULDN’T have different seasons…just the same boring weather all year long. In Texas, it’d be about 90 degrees every ...
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Unit 11: Stellar Evolution
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FAR, FAR AWAY - Museum of Science and Industry
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Energy production in stars
Energy production in stars

... This would be enough to supply the sun’s radiation for 1500 milliards of years. However nobody has ever observed the complete annihilation of matter. From experiments on earth we know that protons and electrons do not annihilate each other in 1030 years. It is hard to believe that the situation woul ...
Basic Information about the Solar System Handout
Basic Information about the Solar System Handout

... Sun's nearest known stellar neighbor is a red dwarf star called Proxima Centauri, at a distance of about 4.2 light years (a light year is the distance light travels in a year, at about 300,000 km per second). We are beginning to find that many stars besides the Sun harbor their own "solar systems" w ...
Astronomy- The Original Science
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... •Newton’s law of gravity explained why all of the planets orbit the most massive object in the solar system---the sun. •Newton once said that “I could see so far because I stood on the shoulders of giants.” He gave credit the observations and ideas of all the scientists who came before him. ...
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... The core is the central region of the Sun and has a temperature of 15 million degrees. From here comes the star’s power; every second 564 million tons of hydrogen are fused, through thermonuclear reactions, to 560 million tons of helium. Hydrogen nuclei (protons) become helium nuclei at a rate of f ...
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
Astronomy 115 Homework Set #1 – Due: Thursday, Feb

... Describe 3 ways that we can observationally probe what is happening inside of stars as they evolve off the main sequence and thereby directly test the predictions of stellar evolution theory. ...
THE SUN IS NOT AN AVERAGE STAR Sometimes biblical creation
THE SUN IS NOT AN AVERAGE STAR Sometimes biblical creation

solar photosphere and chromosphere
solar photosphere and chromosphere

TEKS PDF - Virtual Observatory
TEKS PDF - Virtual Observatory

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–1– 4. Energy transport in stars Stars are hotter at the centre, hence

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... SILICON CRYODETECTOR 15100cc M=3kg, ionization-into-heat conversion effect (CWRU-StanfordJINR) HIGH-PURITY-GERMANIUM DETECTOR 6150cc, M=4.8kg, internal amplification by avalanche multiplication (ITEP) SENSITIVITY (95% C.L.): mn 2.5 10-12mB ...
Ia 超新星的
Ia 超新星的

... When the central density approach the critical value (2109 g cm-3), the thermonuclear reaction rate exceeds the energy loss neutrino the ignition of 12C + 12C takes place in the center due to the compressional heating. The release energy further increases the temperature, thus further accelerating ...
The Formation of the Solar System
The Formation of the Solar System

< 1 ... 128 129 130 131 132 133 134 135 136 ... 237 >

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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