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Astronomy Scavenger Hunt Distances 1. What is the
Astronomy Scavenger Hunt Distances 1. What is the

No Slide Title
No Slide Title

... • The core implodes under the force of gravity. • This implosion is so strong it forces electrons and protons to combine and form neutrons – in a matter of seconds a city sized superdense mass of neutrons is created. • The process involves the weak interaction called “electron capture” ...
Earth Science-FCAT Practice
Earth Science-FCAT Practice

... A. A year on Mars would last almost as long as two Earth years. B. Water would run in the canals on Mars on the warmest days. C. They would see four big moons and several smaller ones at night on Mars. D. They could breathe the air since Mars and Earth have similar atmospheres. 5) When comets come c ...
educator guide - Michigan Science Center
educator guide - Michigan Science Center

... The Sun is humanity’s star. It is classified as a G2V star (see stellar classification) along the main sequence. The Sun was once considered to be a fairly dim star compared to most other stars in the universe. Recent discoveries have shown, however, that there are many more red dwarf stars than exp ...
Lectures 12 & 13 powerpoint (stellar death)
Lectures 12 & 13 powerpoint (stellar death)

... Q: The Helium core contracts and heats the star enough to induce a hydrogen-burning shell… so what stops the helium core from contracting to zero radius (keep in mind that He fusion has not set in yet….)? A: Degeneracy pressure! The core becomes very dense… and two laws of quantum mechanics becom ...
The Sun
The Sun

... The Sun’s Life Cycle • What happens during a star’s life cycle depends on its mass. – It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. – When the hydrogen in its core is gone, a star has a helium center and outer layers made ...
How did the solar system form? (reading
How did the solar system form? (reading

Star Life Cycles Stellar Nebula
Star Life Cycles Stellar Nebula

... Nuclear fusion begins (the power ...
math help sheet - Lawrence University
math help sheet - Lawrence University

... and very small numbers. Scientists have developed a mathematical shortcut for expressing these numbers called scientific notation. To write a number that is greater than 1 in scientific notation, count the number of spaces after the first number (we’ll call it n). Then rewrite the original number by ...
Some Scientific Evidences
Some Scientific Evidences

... Entropy--where the physical universe is reaching toward a condition of greater randomness. It is when a system shifts toward equilibrium in which fewer restrictions are placed on the positions and motion of the atoms and molecules. It is the measure of the unavailable energy in a system. It is the m ...
Frantic Finish - Max-Planck
Frantic Finish - Max-Planck

Planets in the Solar System - Etiwanda E
Planets in the Solar System - Etiwanda E

... made up of water, methane, and ammonia.  The center core is made up of rocky ice. ...
earth in space ppt
earth in space ppt

... of energy by electromagnetic waves • Solar radiation is energy from the Sun. It is a major source of energy on Earth. • The farther away an energy source, the greater its energy output must be to produce the same effect as a closer source. • Earth and its atmosphere absorb and reflect the Sun’s radi ...
nearest star
nearest star

math help sheet - Lawrence University
math help sheet - Lawrence University

... and very small numbers. Scientists have developed a mathematical shortcut for expressing these numbers called scientific notation. To write a number that is greater than 1 in scientific notation, count the number of spaces after the first number (we’ll call it n). Then rewrite the original number by ...
Module 3: Exploring Other Stars Assignment 5: Estimating
Module 3: Exploring Other Stars Assignment 5: Estimating

Objective 1 summary
Objective 1 summary

... not point towards or away from the sun d. Vernal equinox: March 21 or 22; sun’s rays strike Earth at 90 degree angle along the equator; first day of spring in Northern Hemisphere; hours of daylight and darkness are equal around the world; North Pole does not tilt towards or away from sun ...
On the relative influence of initial H2O and CO2 contents on the
On the relative influence of initial H2O and CO2 contents on the

... Estimates of initial volatile contents inside planets primitive magma oceans (hereafter « MO ») varies by several orders of magnitude. However, the release of greenhouse gasses such as H2 O and CO2 during cooling and crystallization of the MO will greatly affect the atmosphere formation, the planet ...
journey to the stars - American Museum of Natural History
journey to the stars - American Museum of Natural History

... Five billion years from now, while the Milky Way is merging with its neighboring galaxy, Andromeda, the Sun will become what is known as a red giant. Nearly all stars do that at the ends of their lives. It’s outer layers will swell towards the Earth. Now don’t worry. This will happen long after huma ...
Slide 1
Slide 1

... Source: Internet Encyclopedia of Science ...
4th Grade Solar System Project
4th Grade Solar System Project

... Families may help students plan, brainstorm ideas and put together their project, but must not do it for them. Students may not buy solar system kits and put them together for their project. The model must be small enough to sit on their desk or be tacked to the wall/hung from the ceiling. Please en ...
Central Temperature and Density of Stars in Gravitational Equilibrium
Central Temperature and Density of Stars in Gravitational Equilibrium

... to hold between the pressure and density throughout the whole interior. Secondly, for a star having a shell structure our consideration is confined to its innermost homogeneous core. The pressure at the core boundary is assumed to be so small compared to the central pressure that the existence of th ...
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 Story of the Solar System Lesson Plan
The Story of the Solar System Lesson Plan

... information about comets, asteroids, and meteoroids.  Photos and images of comets, meteoroids, and asteroids. 1. Divide the class into groups of 4-5 and tell them that they are going to be making poster presentations for the rest of the class. Give them the option of researching asteroids, comets, ...
THE END - SMU Physics
THE END - SMU Physics

< 1 ... 115 116 117 118 119 120 121 122 123 ... 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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