Folie 1
... Evolution to Red Giant • Once the star uses up all the H in its convective core, nuclear fusion ceases, convection is quenched. The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the ...
... Evolution to Red Giant • Once the star uses up all the H in its convective core, nuclear fusion ceases, convection is quenched. The star is no longer in hydrostatic equilibrium. – Gravity wins out over pressure, and the core begins to collapse and heats up. – As the core shrinks, the energy of the ...
Our Galaxy
... This sequence shows how astronomers are using Chandra to help probe the mysterious region at the center of the Milky Way. The first image is a 900- by 400-light-year mosaic in X-rays taken by Chandra. The view then zooms into a smaller region that encompasses the latest Chandra discovery of puzzlin ...
... This sequence shows how astronomers are using Chandra to help probe the mysterious region at the center of the Milky Way. The first image is a 900- by 400-light-year mosaic in X-rays taken by Chandra. The view then zooms into a smaller region that encompasses the latest Chandra discovery of puzzlin ...
G485 5.5.1 Structure of the Universe
... only appears when it is near the Sun and it always points directly away from the Sun. The solar wind, an emission of ions from the Sun’s surface, causes the comet’s gases to spread out, become ionised and therefore glow. ...
... only appears when it is near the Sun and it always points directly away from the Sun. The solar wind, an emission of ions from the Sun’s surface, causes the comet’s gases to spread out, become ionised and therefore glow. ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
The Sun - MsLeeClass
... 2. Reading the following Joke: When people run around and around in circles we say they are crazy. When planets do it we say they are orbiting. 3. Write down one thing you learned from yesterday. MINI-LESSON/MODELLING: 15 min Students will work in partners doing a jig saw lesson Procedure for Jig Sa ...
... 2. Reading the following Joke: When people run around and around in circles we say they are crazy. When planets do it we say they are orbiting. 3. Write down one thing you learned from yesterday. MINI-LESSON/MODELLING: 15 min Students will work in partners doing a jig saw lesson Procedure for Jig Sa ...
large PDF file
... • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of ...
... • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of ...
7.4 Evolution on the Main-Sequence Main-sequence (m
... of m-s evolution. As H is exhausted, the star establishes a H-burning shell source around the core. The m-s lifetime τm−s ∝ M/L and since L ∝ M 3 , then τm−s ∝ M −2 . Massive stars have m-s lifetimes of a few million years compared to 1010 yr for the Sun. The lifetime of a massive star (M > 15 M ) ...
... of m-s evolution. As H is exhausted, the star establishes a H-burning shell source around the core. The m-s lifetime τm−s ∝ M/L and since L ∝ M 3 , then τm−s ∝ M −2 . Massive stars have m-s lifetimes of a few million years compared to 1010 yr for the Sun. The lifetime of a massive star (M > 15 M ) ...
Chapter 20 Notes (smaller PDF file)
... core surrounded by concentric shells hosting the various thermonuclear reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of ...
... core surrounded by concentric shells hosting the various thermonuclear reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of ...
doc - Pocket Stars
... manually from this page. Select the ARM processor. Checking the "SDSS" displays images from the Sloan Digital Sky Survey if you have an internet connection. You can zoom in and out using the "+" and "-" buttons. Note that SDSS does not cover the entire sky: most objects in the range M80 to M100 are ...
... manually from this page. Select the ARM processor. Checking the "SDSS" displays images from the Sloan Digital Sky Survey if you have an internet connection. You can zoom in and out using the "+" and "-" buttons. Note that SDSS does not cover the entire sky: most objects in the range M80 to M100 are ...
Announcements - Lick Observatory
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
... Galaxy, but for the vast majority, the separation of the stars is large enough that one star doesn’t affect the evolution of the other(s). ...
Constraining the formation of the Milky Way: Ages
... We will show that our new approach works encouragingly well, explaining not only current observations, but also leading to a more clear picture regarding the nature of the MW thick disc. The novelty of our approach is: a) we assume that each particle in our N-body simulation represents one star. Dyn ...
... We will show that our new approach works encouragingly well, explaining not only current observations, but also leading to a more clear picture regarding the nature of the MW thick disc. The novelty of our approach is: a) we assume that each particle in our N-body simulation represents one star. Dyn ...
Wien`s law - Uplift Education
... • Perhaps the Universe is not infinite. But current model of the Universe is that it is infinite. • Perhaps the light is absorbed before it gets to us. But then Universe would warm up and eventually reradiate energy. Real help: the Big Bang model leads to the idea that the observable universe is not ...
... • Perhaps the Universe is not infinite. But current model of the Universe is that it is infinite. • Perhaps the light is absorbed before it gets to us. But then Universe would warm up and eventually reradiate energy. Real help: the Big Bang model leads to the idea that the observable universe is not ...
Distances to the Stars in Leo
... Background and Theory If the distance to the star is known via its measured parallax (as it was discussed in class), it is a somewhat easyl matter for astronomers, or anyone else for that matter, to determine the absolute magnitude of the star using the distance-magnitude relation. However, most sta ...
... Background and Theory If the distance to the star is known via its measured parallax (as it was discussed in class), it is a somewhat easyl matter for astronomers, or anyone else for that matter, to determine the absolute magnitude of the star using the distance-magnitude relation. However, most sta ...
7-12 Script - Geophysical Institute
... the terrestrial planets and the asteroid belt. Ask what keeps planets in orbit around the sun (gravitational forces). Our solar system is just a small part of our galaxy, the Milky Way. Show the MILKY WAY FROM SPACE. (or use Fav/Stars/Sun in Milky Way). Just as gravitational forces keep planets in o ...
... the terrestrial planets and the asteroid belt. Ask what keeps planets in orbit around the sun (gravitational forces). Our solar system is just a small part of our galaxy, the Milky Way. Show the MILKY WAY FROM SPACE. (or use Fav/Stars/Sun in Milky Way). Just as gravitational forces keep planets in o ...
Journey to the Stars Educator`s Guide
... a rate one-tenth as high. • About 4.5 billion years ago, within the Milky Way Galaxy, our Sun was born from a dense cloud of gas and dust, along with hundreds to thousands of other stars in a star cluster. As happens with many young stars, our Sun was ejected from its cluster. Since then it has trav ...
... a rate one-tenth as high. • About 4.5 billion years ago, within the Milky Way Galaxy, our Sun was born from a dense cloud of gas and dust, along with hundreds to thousands of other stars in a star cluster. As happens with many young stars, our Sun was ejected from its cluster. Since then it has trav ...
ASTR-264-Lecture
... 3. if Earth were really orbiting sun, we’d detect stellar parallax Oercoming the 1st objection (nature of motion) Galileo’s experiments showed that o bjects in air would stay with a moving earth Aristotle thought all objects naturally come to rest Galileo showed that objects will stay in motions unl ...
... 3. if Earth were really orbiting sun, we’d detect stellar parallax Oercoming the 1st objection (nature of motion) Galileo’s experiments showed that o bjects in air would stay with a moving earth Aristotle thought all objects naturally come to rest Galileo showed that objects will stay in motions unl ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.