Astro 10: Introductory Astronomy
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
Recurring theme: conservation of energy
... C. Gravitational energy that is released as the cloud compresses D. Fusion E. Kinetic energy of all the material falling faster and faster ...
... C. Gravitational energy that is released as the cloud compresses D. Fusion E. Kinetic energy of all the material falling faster and faster ...
Last time: Star Clusters (sec. 19.6)
... Further evolution of low-mass stars: Planetary nebulae, white dwarfs During the entire RG and AGB phases, significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Fig. 20.9 and Discovery 20-2.) The star is also ...
... Further evolution of low-mass stars: Planetary nebulae, white dwarfs During the entire RG and AGB phases, significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Fig. 20.9 and Discovery 20-2.) The star is also ...
1. Introduction
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
Supernovae — Oct 21 10/21/2011 • Outline
... A particle must move if it is confined to a small space. If you confine an electron to 10-8m, it moves at 70km/s. ...
... A particle must move if it is confined to a small space. If you confine an electron to 10-8m, it moves at 70km/s. ...
Lab 9
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
Where Do Baby Stars Come From?
... cause the dark molecular cloud to start spinning. Each of the fragments within it will spin. As they collapse it’s sort of like an ice skater pulling her arms in towards her body. As you get your distribution of mass closer and closer to the centre of the mass, an object spins faster and faster. As ...
... cause the dark molecular cloud to start spinning. Each of the fragments within it will spin. As they collapse it’s sort of like an ice skater pulling her arms in towards her body. As you get your distribution of mass closer and closer to the centre of the mass, an object spins faster and faster. As ...
Star`s ReadingStar`s Reading(es)
... Characteristics of Stars Imagine you could travel to the stars at the speed of light. To travel from Earth to the sun would take about 8 minutes, not very long for such a long trip! Yet the next nearest star, Proxima Centauri, is much farther away—a trip to Proxima Centauri would take 4.2 years! ...
... Characteristics of Stars Imagine you could travel to the stars at the speed of light. To travel from Earth to the sun would take about 8 minutes, not very long for such a long trip! Yet the next nearest star, Proxima Centauri, is much farther away—a trip to Proxima Centauri would take 4.2 years! ...
Space Explorations - Holy Cross Collegiate
... • The spectrum of an approaching star shows the dark bands shifting to the blue end of the spectrum, whereas, the shift is to the red part of the spectrum if a star is moving away from the Earth • The amount of shift indicates the speed at which the ...
... • The spectrum of an approaching star shows the dark bands shifting to the blue end of the spectrum, whereas, the shift is to the red part of the spectrum if a star is moving away from the Earth • The amount of shift indicates the speed at which the ...
Luminosity Classes
... These are called Variable Stars. The change in luminosity is due to a change in size. (Though temperature changes too.) ...
... These are called Variable Stars. The change in luminosity is due to a change in size. (Though temperature changes too.) ...
Lecture 4-Energy sources
... Aims and outline for this lecture • describe energy sources of astronomical objects ...
... Aims and outline for this lecture • describe energy sources of astronomical objects ...
General Introduction 1. Luminosity, Flux and Magnitude The
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
Star Classification - University of Louisville
... surface temperatures are much higher, and shine white instead of red. When the Sun comes to the end of its life, it will become a White Dwarf. It will be much smaller than it is now, not quite as bright but twice as hot. Its matter (particles) will be more densely-packed together. ...
... surface temperatures are much higher, and shine white instead of red. When the Sun comes to the end of its life, it will become a White Dwarf. It will be much smaller than it is now, not quite as bright but twice as hot. Its matter (particles) will be more densely-packed together. ...
Galaxies Galore
... that are interacting or colliding may be referred to as a pair, or one galaxy may be referred to as a companion of the other. These HST images show how different colliding galaxies can look. The appearance of an interacting system of galaxies depends on many factors, including the number of galaxies ...
... that are interacting or colliding may be referred to as a pair, or one galaxy may be referred to as a companion of the other. These HST images show how different colliding galaxies can look. The appearance of an interacting system of galaxies depends on many factors, including the number of galaxies ...
PowerPoint Presentation - Research in observational
... • Bottleneck: there are no stable elements of mass number 5 or 8, so He + p, or He + He, likely to happen in an H and He-rich environment, end up in products that vanish immediately. • As the Tc rises 8Be, although unstable, can be formed at a rate high enough to result in a non zero abundance of th ...
... • Bottleneck: there are no stable elements of mass number 5 or 8, so He + p, or He + He, likely to happen in an H and He-rich environment, end up in products that vanish immediately. • As the Tc rises 8Be, although unstable, can be formed at a rate high enough to result in a non zero abundance of th ...
Test 3 Review
... Emission Nebulae or H II Regions Regions of gas and dust near stars just formed. The Hydrogen is essentially fully ionized. Temperatures near 10,000 K ...
... Emission Nebulae or H II Regions Regions of gas and dust near stars just formed. The Hydrogen is essentially fully ionized. Temperatures near 10,000 K ...
Chapter 20 Stellar Evolution (20.1-20.3)
... There is no more outward fusion pressure being generated in the core, which continues to contract. The outer layers become unstable and are eventually ejected. ...
... There is no more outward fusion pressure being generated in the core, which continues to contract. The outer layers become unstable and are eventually ejected. ...
Spiral Galaxies: Density Waves
... explode. The brightest (and bluest) of a galaxy’s stars will never be far from the spiral arm where they were born. ...
... explode. The brightest (and bluest) of a galaxy’s stars will never be far from the spiral arm where they were born. ...
Class 28 (Jun 2) - Physics at Oregon State University
... gravitational pull can tear both galaxies apart. • This can occur with no stars actually colliding! (The space is so enormous!) • Eventually, a new elliptical galaxy will form… ...
... gravitational pull can tear both galaxies apart. • This can occur with no stars actually colliding! (The space is so enormous!) • Eventually, a new elliptical galaxy will form… ...
Measuring Distance with Spectroscopic Parallax
... Where L is in Watts, B is in Watts per square meter, and d comes out in meters. 1. Using the given brightness (in Watts per square meter) and the luminosities you found (in Watts), calculate the distance to each star and record the distances (in meters) in Table 1. 2. There are 9.46!1015 meters in o ...
... Where L is in Watts, B is in Watts per square meter, and d comes out in meters. 1. Using the given brightness (in Watts per square meter) and the luminosities you found (in Watts), calculate the distance to each star and record the distances (in meters) in Table 1. 2. There are 9.46!1015 meters in o ...
Galaxy Classification Much of modern extragalactic astronomy deals
... An interesting system that is still (partially) with us and has (some) interesting uses is the classification system of Morgan. The system has two components, a “concentration” component, and a “form” component. The concentration part of the system is the observed correlation between the types of s ...
... An interesting system that is still (partially) with us and has (some) interesting uses is the classification system of Morgan. The system has two components, a “concentration” component, and a “form” component. The concentration part of the system is the observed correlation between the types of s ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.