Chapter 12
... They emit line radiation (hot, low pressure gas) but in size they are much smaller than the emission nebulae (HII regions) ...
... They emit line radiation (hot, low pressure gas) but in size they are much smaller than the emission nebulae (HII regions) ...
Where planets are formed: Protoplanetary disk evolution and planet
... Nebula distance from supernova < 0.3 pc N>1000 • The Solar System survived the supernova explosion distance from the supernova > 0.1 pc Solar System properties require the Sun formed in the outer region of an intermediate massive cluster, with few thousand members, necessary to provide the req ...
... Nebula distance from supernova < 0.3 pc N>1000 • The Solar System survived the supernova explosion distance from the supernova > 0.1 pc Solar System properties require the Sun formed in the outer region of an intermediate massive cluster, with few thousand members, necessary to provide the req ...
Stars: from Adolescence to Old Age
... Shell burning starts •outer layers of star expand •core continues to contract ...
... Shell burning starts •outer layers of star expand •core continues to contract ...
E1 Introduction to the universe
... An open Universe is one that continues to expand forever. The force of gravity slows the rate of recession of the galaxies down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses ba ...
... An open Universe is one that continues to expand forever. The force of gravity slows the rate of recession of the galaxies down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses ba ...
14-1 Reading Questions: Neutron Stars
... 1. A neutron star, containing a little more than _________ solar mass, compressed to a radius of about __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a __________________ ...
... 1. A neutron star, containing a little more than _________ solar mass, compressed to a radius of about __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a __________________ ...
28. What causes waves - Summer Science Safari
... apparent magnitude how bright a star appears from earth galaxy largest grouping of stars in space absolute magnitude the actual brightness of a star parallax one of the ways we measure distances in space; apparent shift in a star’s location nebulae cloud of hyrdogen gas and dust; birthplace of stars ...
... apparent magnitude how bright a star appears from earth galaxy largest grouping of stars in space absolute magnitude the actual brightness of a star parallax one of the ways we measure distances in space; apparent shift in a star’s location nebulae cloud of hyrdogen gas and dust; birthplace of stars ...
Mass and the Properties of Main Sequence Stars
... neutrons, and releasing neutrinos and energy at the same time Supernova explosion. Eventually the neutron degeneracy pressure will balance the gravitational pressure (if the star is not too massive) to form a neutron star. The estimated of the neutron stars are about 10 km in diameter, with a mass ...
... neutrons, and releasing neutrinos and energy at the same time Supernova explosion. Eventually the neutron degeneracy pressure will balance the gravitational pressure (if the star is not too massive) to form a neutron star. The estimated of the neutron stars are about 10 km in diameter, with a mass ...
April - Bristol Astronomical Society
... 1845 by Lord Rosse, who made a very careful and accurate painting. This face on spiral is one of the showpiece objects of the spring sky and is an easy object to locate as it lies just to the Southwest of eta (η) UMa, the end star in the handle of “the plough”. At magnitude 8.4, it should be visible ...
... 1845 by Lord Rosse, who made a very careful and accurate painting. This face on spiral is one of the showpiece objects of the spring sky and is an easy object to locate as it lies just to the Southwest of eta (η) UMa, the end star in the handle of “the plough”. At magnitude 8.4, it should be visible ...
Chapter 27 Quasars, Active Galaxies, and Gamma
... • Quasars have 100 times the luminosity of our Galaxy • The engine powering quasars is only a few light years across • The only known engine which is powerful enough and compact enough is a black hole • Quasars contain supermassive black holes ...
... • Quasars have 100 times the luminosity of our Galaxy • The engine powering quasars is only a few light years across • The only known engine which is powerful enough and compact enough is a black hole • Quasars contain supermassive black holes ...
Search for Student Research Assistant
... (Sco X-1 for short) is a double star system. It’s actually the brightest spot in the sky in X-rays (other than the Sun). Of the two stars, one is a normal star, slightly less massive than our own Sun, but the other is a neutron star (a collapsed star only about 10 km across). Sco X-1 was the first d ...
... (Sco X-1 for short) is a double star system. It’s actually the brightest spot in the sky in X-rays (other than the Sun). Of the two stars, one is a normal star, slightly less massive than our own Sun, but the other is a neutron star (a collapsed star only about 10 km across). Sco X-1 was the first d ...
Open Houses at the Campus Observatory Astronomical Horizons Lecture
... The sun becomes degenerate The sun loses too much mass as a planetary nebula It takes too long to burn neon. ...
... The sun becomes degenerate The sun loses too much mass as a planetary nebula It takes too long to burn neon. ...
Astronomy In the News Parallax Class demos: Parallax
... Brad and Angelina are two stars that have the same apparent brightness. Brad has a larger parallactic angle than Angelina. Which star is more luminous? ...
... Brad and Angelina are two stars that have the same apparent brightness. Brad has a larger parallactic angle than Angelina. Which star is more luminous? ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... • Astronomers determine the mass of a star by examining how strong the gravitational field is around that star. (Isaac Newton’s law of universal gravitation; §4-7) • By studying the motion of planets around our Sun, astronomers have determined that the Sun has a mass of 2 x 1030 kilograms. • We cann ...
... • Astronomers determine the mass of a star by examining how strong the gravitational field is around that star. (Isaac Newton’s law of universal gravitation; §4-7) • By studying the motion of planets around our Sun, astronomers have determined that the Sun has a mass of 2 x 1030 kilograms. • We cann ...
ph507lecnote06
... Helium shell burning, like the hydrogen shell before it, heats the outer layers of the star and it expands again to form a red supergiant. ...
... Helium shell burning, like the hydrogen shell before it, heats the outer layers of the star and it expands again to form a red supergiant. ...
Slide 1
... How do stars end? • Eventually all hydrogen in the Sun’s core will be used up • As fusion slows down in the core of any star, its core cools down and there is less pressure, so the core collapses • The star’s out layers, which contain hydrogen, fall inwards, becoming hot • This causes new fusion re ...
... How do stars end? • Eventually all hydrogen in the Sun’s core will be used up • As fusion slows down in the core of any star, its core cools down and there is less pressure, so the core collapses • The star’s out layers, which contain hydrogen, fall inwards, becoming hot • This causes new fusion re ...
Is the Sun a Star? - Classroom Websites
... each planetary system has a central starjust as our own solar system has one star, sometimes called by its Roman name, Sol. In some systems there are two (or even more stars) at the center. • Another approach, appropriate for middle and high school levels, is to have students research the history of ...
... each planetary system has a central starjust as our own solar system has one star, sometimes called by its Roman name, Sol. In some systems there are two (or even more stars) at the center. • Another approach, appropriate for middle and high school levels, is to have students research the history of ...
PPT - IAC
... 2.- This is a process that happens at all redshifts, including the local universe. Solid theoretical prediction 3.- XMP galaxies seems to be primitive disks in the process of assembling in the nearby universe, where a major cold-flow accretion episode is producing the current starburst. 4.- XMP seem ...
... 2.- This is a process that happens at all redshifts, including the local universe. Solid theoretical prediction 3.- XMP galaxies seems to be primitive disks in the process of assembling in the nearby universe, where a major cold-flow accretion episode is producing the current starburst. 4.- XMP seem ...
The Luminosity
... Fusion is a lot harder to achieve than fission, because like charges repel. If you try to shove two hydrogen nuclei together--each consisting of a single positively charged proton--they're not going to like it. The sun overcomes this by cramming everything together to a density 100 times that of wat ...
... Fusion is a lot harder to achieve than fission, because like charges repel. If you try to shove two hydrogen nuclei together--each consisting of a single positively charged proton--they're not going to like it. The sun overcomes this by cramming everything together to a density 100 times that of wat ...
stars-notes
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
Study Guide for 1ST Astronomy Exam
... Unit 33: The Origin of the Solar System Describe the three basic ingredients of the “cosmic cupboard” and how these three ingredients and the thermal structure of the solar nebula create the distribution of planets that we see in our solar system. Describe the steps in the formation of solar sy ...
... Unit 33: The Origin of the Solar System Describe the three basic ingredients of the “cosmic cupboard” and how these three ingredients and the thermal structure of the solar nebula create the distribution of planets that we see in our solar system. Describe the steps in the formation of solar sy ...
Deaths of Stars - Chabot College
... Determined it was 300 pc away. They called it a “pulsar”, but what was it? ...
... Determined it was 300 pc away. They called it a “pulsar”, but what was it? ...
The classification of stellar spectra
... - neutral element: H I, He I, Fe I, etc. - single-ionized element: H II, O II, etc. - double-ionized element: O III, etc. ...
... - neutral element: H I, He I, Fe I, etc. - single-ionized element: H II, O II, etc. - double-ionized element: O III, etc. ...
Bolte_LRIS_08A
... dSph-to-dSph differences in the metallicity distributions, which suggests a wide variety of star formation and chemical enrichment histories. In the dSph there is also a strong deficiency of stars with [Fe/H]<-3.0 dex compared to the Galactic halo. These finding seem to challenge the idea that dSph ...
... dSph-to-dSph differences in the metallicity distributions, which suggests a wide variety of star formation and chemical enrichment histories. In the dSph there is also a strong deficiency of stars with [Fe/H]<-3.0 dex compared to the Galactic halo. These finding seem to challenge the idea that dSph ...
Lecture 21 (pdf from the powerpoint)
... • This technique allows us to see galaxies at various stages of formation • These early galaxies tend to be smaller than the Milky Way, and to not fall into Hubble’s classification scheme ...
... • This technique allows us to see galaxies at various stages of formation • These early galaxies tend to be smaller than the Milky Way, and to not fall into Hubble’s classification scheme ...
CASPEC Observations of the Most Metal-Deficient Main
... does not lie in an obscured region, and (2) it does not illuminate fairly bright nebulosity in its immediate vicinity. Moreover, N82 is too bright to be a Herbig AelBe star. Strom et al. (1972) give a list of 12 Galactic stars of this type with known distances. If we place these stars in the SMC, th ...
... does not lie in an obscured region, and (2) it does not illuminate fairly bright nebulosity in its immediate vicinity. Moreover, N82 is too bright to be a Herbig AelBe star. Strom et al. (1972) give a list of 12 Galactic stars of this type with known distances. If we place these stars in the SMC, th ...
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.