Examples - University of Waterloo
... A photon with wavelength less than this can ionize H no matter what level the electron is initially in. ...
... A photon with wavelength less than this can ionize H no matter what level the electron is initially in. ...
The solar system rotates around the sun due to the sun`s
... When we look into the universe and see that all galaxies have a red shift. What does this tell us about the universe? A ...
... When we look into the universe and see that all galaxies have a red shift. What does this tell us about the universe? A ...
SPA 302: THE EVOLUTION OF STARS LECTURE 1: BASICS OF
... 1.3.2 Brightness and Luminosity of Stars The luminosity of a star, denoted by L, is one of the most important characteristics of stars. It is measured in Watts (W) or as a multiple of the Sun's luminosity Lʘ and it is the amount of energy emitted per unit are of a star surface per second. However, i ...
... 1.3.2 Brightness and Luminosity of Stars The luminosity of a star, denoted by L, is one of the most important characteristics of stars. It is measured in Watts (W) or as a multiple of the Sun's luminosity Lʘ and it is the amount of energy emitted per unit are of a star surface per second. However, i ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University Tel.: 08-6428226 Email: [email protected] ...
... AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University Tel.: 08-6428226 Email: [email protected] ...
Ch 20 Notes Stars
... “Recognize that the very molecules that make up your body, the atoms that construct the molecules, are traceable to the crucibles that were once the centers of high mass stars that exploded their chemically rich guts into the galaxy, enriching pristine gas clouds with the chemistry of life. So that ...
... “Recognize that the very molecules that make up your body, the atoms that construct the molecules, are traceable to the crucibles that were once the centers of high mass stars that exploded their chemically rich guts into the galaxy, enriching pristine gas clouds with the chemistry of life. So that ...
dark matter
... Cepheids are one of the most important of the standard candles – objects whose absolute magnitude is known and so whose distance can easily be found. Other examples of standard candles are: RR Lyrae stars (similar to Cepheids but less luminous) planetary nebulae Type Ia supernovae We talked about co ...
... Cepheids are one of the most important of the standard candles – objects whose absolute magnitude is known and so whose distance can easily be found. Other examples of standard candles are: RR Lyrae stars (similar to Cepheids but less luminous) planetary nebulae Type Ia supernovae We talked about co ...
Slides from the first lecture
... Nuclear energy: fusion • In contrast with chemical reactions, nuclear reactions (which change one type of nucleus into another) typically release energies in the MeV range, 1 million times larger. • E.g. Assume the Sun was originally 100% hydrogen, and converted the central 10% of H into helium. • ...
... Nuclear energy: fusion • In contrast with chemical reactions, nuclear reactions (which change one type of nucleus into another) typically release energies in the MeV range, 1 million times larger. • E.g. Assume the Sun was originally 100% hydrogen, and converted the central 10% of H into helium. • ...
The Cosmic Near-Infrared Background: Remnant light form
... absolute photometry imaging and spectroscopy experiment optimized to detect signatures of first-light galaxies present during reionization in the unresolved IR background. CIBER-I consists of a wide-field two-color camera for fluctuation measurements, a low-resolution absolute spectrometer for absol ...
... absolute photometry imaging and spectroscopy experiment optimized to detect signatures of first-light galaxies present during reionization in the unresolved IR background. CIBER-I consists of a wide-field two-color camera for fluctuation measurements, a low-resolution absolute spectrometer for absol ...
Week 1b_2015
... In contrast to chemical reactions which involve sharing of electrons in different atoms and can readily occur at room temperature, nuclear reactions require extreme temperatures (i.e., > 50 million degrees) and pressures to fuse nuclei (e.g., to overcome the electrical repulsion exerted by one proto ...
... In contrast to chemical reactions which involve sharing of electrons in different atoms and can readily occur at room temperature, nuclear reactions require extreme temperatures (i.e., > 50 million degrees) and pressures to fuse nuclei (e.g., to overcome the electrical repulsion exerted by one proto ...
Unit Two Worksheet – Astronomy
... Testing of a hypothesis for validity Large system of stars and planets Apparent shift in the wavelength of energy emitted by a source moving away from or toward an observer Produced when light is passed through a prism, the production of a band of the various colors of light Hypothesis or set of hyp ...
... Testing of a hypothesis for validity Large system of stars and planets Apparent shift in the wavelength of energy emitted by a source moving away from or toward an observer Produced when light is passed through a prism, the production of a band of the various colors of light Hypothesis or set of hyp ...
4. Sketch and label the life cycle of a star. Give a short phrase
... Mass – A measure of how much matter an object contains. It is a property of the object and not affected by gravity. Your mass is the same, no matter where you are in the universe! Weight – The resulting force of the gravitational pull on an object. You will weigh less on the moon because there is le ...
... Mass – A measure of how much matter an object contains. It is a property of the object and not affected by gravity. Your mass is the same, no matter where you are in the universe! Weight – The resulting force of the gravitational pull on an object. You will weigh less on the moon because there is le ...
Unit 3 - Lesson 8.9 Life of Stars Challenge
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
... These coloured Super Giants have luminosities often 1,000,000X greater than the Sun The explosive death of a star A cloud of hydrogen gas and dust in space. When the gravitational and pressure forces within the initial cloud become unbalanced, the cloud collapses and breaks into small fragments. The ...
the summary
... In the core of a star, hydrogen particles are fused into helium. After that, when the core contracts a bit, this helium can further fuse to heavier elements such as carbon, nitrogen and oxygen. In the most massive stars this can continue until the core consists of iron. Around the core, there will b ...
... In the core of a star, hydrogen particles are fused into helium. After that, when the core contracts a bit, this helium can further fuse to heavier elements such as carbon, nitrogen and oxygen. In the most massive stars this can continue until the core consists of iron. Around the core, there will b ...
here - Next Wave
... At this point there was nothing on Earth even remotely resembling life. But thanks to the stellar furnaces that had worked unceasingly for billions of years, our planet was replete with oxygen, carbon, nitrogen, and all the other materials needed for living creatures to someday emerge. The Big Bang, ...
... At this point there was nothing on Earth even remotely resembling life. But thanks to the stellar furnaces that had worked unceasingly for billions of years, our planet was replete with oxygen, carbon, nitrogen, and all the other materials needed for living creatures to someday emerge. The Big Bang, ...
sc_examII_spring_2002 - University of Maryland Astronomy
... E. red shifted 2. The smaller the parallax angle for a star, A. the less massive the star. B. the more massive the star. C. the smaller the distance to the star. D. the greater the distance to the star. E. both A and C 3. By combining information from both the light curve and spectrum of Algol, the ...
... E. red shifted 2. The smaller the parallax angle for a star, A. the less massive the star. B. the more massive the star. C. the smaller the distance to the star. D. the greater the distance to the star. E. both A and C 3. By combining information from both the light curve and spectrum of Algol, the ...
Chapter 12
... 1. The temperature of a star can be determined from its_____________. 2. The pattern of the absorption spectral lines for a star contains information about a star’s________________. 3. The Doppler shift of a star's spectral lines tells us something about the star’s_______________. 4. The distance of ...
... 1. The temperature of a star can be determined from its_____________. 2. The pattern of the absorption spectral lines for a star contains information about a star’s________________. 3. The Doppler shift of a star's spectral lines tells us something about the star’s_______________. 4. The distance of ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.