Measuring Stars
... •Observe the star – determine it’s brightness B •Measure its spectral type from spectrum •Deduce its luminosity from the HertzsprungRussell Diagram •Find its distance from: L = 4d2B ...
... •Observe the star – determine it’s brightness B •Measure its spectral type from spectrum •Deduce its luminosity from the HertzsprungRussell Diagram •Find its distance from: L = 4d2B ...
ppt - Astronomy & Physics
... spectrum passes through cool gas, dark lines appear in the continuous spectrum. Such “cool” gas exists in outer layers of stars, absorbing light at certain wavelengths from continuous spectrum coming from below. ...
... spectrum passes through cool gas, dark lines appear in the continuous spectrum. Such “cool” gas exists in outer layers of stars, absorbing light at certain wavelengths from continuous spectrum coming from below. ...
Chapter15 (with interactive links)
... The stars in globular clusters in the halo have some heavy elements, so at least one prior generation of stars must have existed. Halo objects were formed before interstellar gas was all concentrated into the disk. Later star formation has been concentrated in the disk. ...
... The stars in globular clusters in the halo have some heavy elements, so at least one prior generation of stars must have existed. Halo objects were formed before interstellar gas was all concentrated into the disk. Later star formation has been concentrated in the disk. ...
Background Information on Galaxy Classification
... Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Inter ...
... Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Inter ...
Maximum Mass Limit of Stars on the Main Sequence
... Competitive accretion is also a viable method for creation of massive stars. Bonnell presents 3D simulations of stellar mass growth by competitive accretion in small young clusters. In this method, growth is promoted by the size and composition of the stars accretion domain. As mass increases, the ...
... Competitive accretion is also a viable method for creation of massive stars. Bonnell presents 3D simulations of stellar mass growth by competitive accretion in small young clusters. In this method, growth is promoted by the size and composition of the stars accretion domain. As mass increases, the ...
Exercise 8
... 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? ...
The Spectra of Stars
... • Visible Visible Hydrogen absorption lines come from Hydrogen absorption lines come from the second excited state. • B B Stars (15‐30,000 K): Stars (15 30 000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): A Stars (10 000 K): Ideal excitation conditions, strongest H lin ...
... • Visible Visible Hydrogen absorption lines come from Hydrogen absorption lines come from the second excited state. • B B Stars (15‐30,000 K): Stars (15 30 000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): A Stars (10 000 K): Ideal excitation conditions, strongest H lin ...
Refuges for Life in a - University of Arizona
... the stars, enriching their metal content. Most astronomers now think that stars do gobble up planets and smaller bodies. But the outer convective layers of sunlike stars are so massive and so well mixed that they would need to devour an unreasonable amount of planetary material to fully account for ...
... the stars, enriching their metal content. Most astronomers now think that stars do gobble up planets and smaller bodies. But the outer convective layers of sunlike stars are so massive and so well mixed that they would need to devour an unreasonable amount of planetary material to fully account for ...
answers
... distant objects ever found. All of the objects are galaxies of stars except for E, which is a single nearby star. Which object is more luminous? A) E B) F C) they are about the same B) The two objects look equally bright, but are very different. The star is much closer and much less luminous. The ga ...
... distant objects ever found. All of the objects are galaxies of stars except for E, which is a single nearby star. Which object is more luminous? A) E B) F C) they are about the same B) The two objects look equally bright, but are very different. The star is much closer and much less luminous. The ga ...
Luminosity
... The stars are not randomly distributed on the diagram. There are 3 features that emerge from the H-R diagram: Most stars fall on a strip extending diagonally across the diagram from top left to bottom right. This is called the MAIN SEQUENCE. Some large stars, reddish in colour occupy the top ...
... The stars are not randomly distributed on the diagram. There are 3 features that emerge from the H-R diagram: Most stars fall on a strip extending diagonally across the diagram from top left to bottom right. This is called the MAIN SEQUENCE. Some large stars, reddish in colour occupy the top ...
May 2013 - Otterbein
... Where does the Energy come from? • Anaxagoras (500-428 BC): Sun a large hot rock – No, it would cool down too fast • Combustion? – No, it could last a few thousand years ...
... Where does the Energy come from? • Anaxagoras (500-428 BC): Sun a large hot rock – No, it would cool down too fast • Combustion? – No, it could last a few thousand years ...
Massive star formation in 100000 years from turbulent and
... rate of the star; the value of the former quantity is currently uncertain by many orders of magnitude1,2,3,4,5,6 , leading to other astrophysical questions. For example, the variation of t∗f with stellar mass dictates whether massive stars can form simultaneously with low-mass stars in clusters. Her ...
... rate of the star; the value of the former quantity is currently uncertain by many orders of magnitude1,2,3,4,5,6 , leading to other astrophysical questions. For example, the variation of t∗f with stellar mass dictates whether massive stars can form simultaneously with low-mass stars in clusters. Her ...
(as Main Sequence Stars)?
... Determine luminosity from apparent brightness and distance, determine temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
... Determine luminosity from apparent brightness and distance, determine temperature from spectrum (black-body curve or spectral lines), then find surface area, then find radius (sphere surface area is 4 p R2) ...
Stars III The Hertzsprung
... light, dust grains are very efficient at absorbing and scattering visible (and even IR) light • Furthermore, the degree to which light is scattered is a function of wavelength: bluer light is scattered much more than redder light (Scattering Demo) ...
... light, dust grains are very efficient at absorbing and scattering visible (and even IR) light • Furthermore, the degree to which light is scattered is a function of wavelength: bluer light is scattered much more than redder light (Scattering Demo) ...
Name: Astronomy Lab: The Hertzsprung-Russell (H
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
chapter8
... intrinsic brightness or luminosity (L) and inversely proportional to the square of the distance (d): L ...
... intrinsic brightness or luminosity (L) and inversely proportional to the square of the distance (d): L ...
Name Physics 130 Astronomy Exam 2 August 2, 2004 Multiple Choice
... a.) a much brighter emission of light from it. b.) its very powerful magnetic field. c.) a coronal hole existing above it. d.) faster rotation around the Sun’s axis than neighboring regions. 16. _____ A positron is a.) a hydrogen nucleus. b.) a positively charged electron. c.) a charged neutron. d.) ...
... a.) a much brighter emission of light from it. b.) its very powerful magnetic field. c.) a coronal hole existing above it. d.) faster rotation around the Sun’s axis than neighboring regions. 16. _____ A positron is a.) a hydrogen nucleus. b.) a positively charged electron. c.) a charged neutron. d.) ...
Activity: Star Classification - d
... Part 1: Exploring with Classification Each group will receive 1 set of 27 stars. Every star has: a color, name, temperature, size, & luminosity value o The luminosity is compared to the sun's luminosity. If a star has a luminosity value of 5, then it is 5 times brighter than our sun. If a star h ...
... Part 1: Exploring with Classification Each group will receive 1 set of 27 stars. Every star has: a color, name, temperature, size, & luminosity value o The luminosity is compared to the sun's luminosity. If a star has a luminosity value of 5, then it is 5 times brighter than our sun. If a star h ...
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 ...
Astronomy Chapter 16 – The Milky Way Galaxy A. Main Ideas 1
... ⇒ Interstellar gas is the material from which stars form, and it is the repository (storage place) of matter blown off dying stars 5. Motion of Stars and Gas in the Milky Way Although all stars within the Milky Way move around its center, the paths followed by stars in the disk and halo are very dif ...
... ⇒ Interstellar gas is the material from which stars form, and it is the repository (storage place) of matter blown off dying stars 5. Motion of Stars and Gas in the Milky Way Although all stars within the Milky Way move around its center, the paths followed by stars in the disk and halo are very dif ...
Dark Matter: Observational Constraints Properties of Dark Matter:
... • This much HI is easily observed in the 21-cm line of atomic hydrogen • Hot, X-ray emitting gas is observed to be insufficient • Warm, 104 K ionized gas emits by bremstrahlung. If in hydrostatic equilibrium, central regions would be dense enough to be easily observed. • Molecular gas must be H2; la ...
... • This much HI is easily observed in the 21-cm line of atomic hydrogen • Hot, X-ray emitting gas is observed to be insufficient • Warm, 104 K ionized gas emits by bremstrahlung. If in hydrostatic equilibrium, central regions would be dense enough to be easily observed. • Molecular gas must be H2; la ...
2. Stellar Physics
... Problem of stellar structure is simplified by making several reasonable assumptions, which hold in most (not all) cases. 1) Spherical symmetry An isolated, non-rotating star which does not contain strong magnetic fields will be spherically symmetric, i.e.: All quantities (e.g. density, temperature, ...
... Problem of stellar structure is simplified by making several reasonable assumptions, which hold in most (not all) cases. 1) Spherical symmetry An isolated, non-rotating star which does not contain strong magnetic fields will be spherically symmetric, i.e.: All quantities (e.g. density, temperature, ...
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 ...
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.