MASSACHUSETTS INSTITUTE OF TECHNOLOGY
... where vr is the radial velocity. (b) Assume that the original cloud had a mass of 1M� and a radius of 0.5 pc. If the collapse is halted at a radius of approximately 100 AU, find the initial angular velocity of the cloud. What was the original rotational velocity (in cm s−1 ) of the edge of the cloud? ...
... where vr is the radial velocity. (b) Assume that the original cloud had a mass of 1M� and a radius of 0.5 pc. If the collapse is halted at a radius of approximately 100 AU, find the initial angular velocity of the cloud. What was the original rotational velocity (in cm s−1 ) of the edge of the cloud? ...
PHYS3380_102815_bw - The University of Texas at Dallas
... that rises slightly will find itself in an environment of lower pressure than the one it came from. As a result, the parcel will expand and cool. If the rising parcel cools to a lower temperature than its new surroundings, so that it has a higher density than the surrounding gas, then its lack of ...
... that rises slightly will find itself in an environment of lower pressure than the one it came from. As a result, the parcel will expand and cool. If the rising parcel cools to a lower temperature than its new surroundings, so that it has a higher density than the surrounding gas, then its lack of ...
SIMPLE RADIATION TRANSFER FOR SPHERICAL STARS
... Inside a star conditions are very close to LTE, but there must be some anisotropy of the radiation field if there is a net flow of radiation from the deep interior towards the surface. We shall consider intensity of radiation as a function of radiation frequency, position inside a star, and a direct ...
... Inside a star conditions are very close to LTE, but there must be some anisotropy of the radiation field if there is a net flow of radiation from the deep interior towards the surface. We shall consider intensity of radiation as a function of radiation frequency, position inside a star, and a direct ...
Massive star formation in 100000 years from turbulent and
... AV = (NH /2 × 1021 cm−2 ) mag = 214 Σ mag, with a dispersion of a factor of a few. These column densities ...
... AV = (NH /2 × 1021 cm−2 ) mag = 214 Σ mag, with a dispersion of a factor of a few. These column densities ...
Stellar Evolution
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
1 Introduction - High Point University
... luminosity), with the same temperature as cooler main sequence stars, have greater surface areas (larger radii). Also, stars that have the same luminosity as dimmer main sequence stars, but are to the left of them (hotter) on the H-R diagram, have smaller surface areas (smaller radii). Bright, cool ...
... luminosity), with the same temperature as cooler main sequence stars, have greater surface areas (larger radii). Also, stars that have the same luminosity as dimmer main sequence stars, but are to the left of them (hotter) on the H-R diagram, have smaller surface areas (smaller radii). Bright, cool ...
Life Cycle of Stars
... through gravity. Once the pressure inside the clump is high enough, hydrogen nuclei join to form helium nuclei through nuclear fusion, and a star is born. Nuclear fusion is the process by which lighter elements combine to form heavier elements. (For example, Hydrogen fuses to form Helium.) This proc ...
... through gravity. Once the pressure inside the clump is high enough, hydrogen nuclei join to form helium nuclei through nuclear fusion, and a star is born. Nuclear fusion is the process by which lighter elements combine to form heavier elements. (For example, Hydrogen fuses to form Helium.) This proc ...
Post main sequence evolution
... This is due to the fact that mass is related to the lifetime of a star. How old is this cluster? 10 billion years! Because stars that live only 10 billion years are just leaving the main sequence. ...
... This is due to the fact that mass is related to the lifetime of a star. How old is this cluster? 10 billion years! Because stars that live only 10 billion years are just leaving the main sequence. ...
click here
... • Hot, massive stars end up in the upper left; cool, low mass stars end up in the lower right. • In addition, there are poorly populated areas. One, in the lower left, is populated by hot, very tiny stars (white dwarfs). Another, in the upper right, is populated by giant stars on the giant branch (p ...
... • Hot, massive stars end up in the upper left; cool, low mass stars end up in the lower right. • In addition, there are poorly populated areas. One, in the lower left, is populated by hot, very tiny stars (white dwarfs). Another, in the upper right, is populated by giant stars on the giant branch (p ...
Astronomy C - Scioly.org
... 71. A star is observed to have an apparent magnitude of +7.3, and we know from other methods that this star has an absolute magnitude of –2.4. a. What is the distance to this star, in pc? b. We realize that a nebula 200 pc thick is between us and the star, causing 1.5 magnitudes of extinction per kp ...
... 71. A star is observed to have an apparent magnitude of +7.3, and we know from other methods that this star has an absolute magnitude of –2.4. a. What is the distance to this star, in pc? b. We realize that a nebula 200 pc thick is between us and the star, causing 1.5 magnitudes of extinction per kp ...
RachelStarProject
... Low-mass stars and high-mass stars take different paths at the end of their lives because high-mass stars become so compact that they have to do something different than low-mass stars. ...
... Low-mass stars and high-mass stars take different paths at the end of their lives because high-mass stars become so compact that they have to do something different than low-mass stars. ...
Stellar Lifetime - Madison Public Schools
... – Cooler surface is becoming opaque to interior radiation – Luminosity is very high because of its size ...
... – Cooler surface is becoming opaque to interior radiation – Luminosity is very high because of its size ...
Part 1: Elements and light
... 5. How is the colored light produced? This really involves 2 things we studied this year…electrons/energy levels (pg. 107) and star color (pg. 669). ...
... 5. How is the colored light produced? This really involves 2 things we studied this year…electrons/energy levels (pg. 107) and star color (pg. 669). ...
Paper
... development are known as the rebirth of a giant star. This article will discuss the life of one very important star, Sakurai’s Object and the converse that surrounds it. There are only three stars that have been observed while in the act of a fast stellar evolution, F.G. Sagittac, V605 Aquilae, and ...
... development are known as the rebirth of a giant star. This article will discuss the life of one very important star, Sakurai’s Object and the converse that surrounds it. There are only three stars that have been observed while in the act of a fast stellar evolution, F.G. Sagittac, V605 Aquilae, and ...
PART II: Life of a Star
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
Stellar Populations of Galaxies- 2 Lectures H
... Classical indicators of what is going on: The limit of the Balmer series and the blending of the high-order Balmer lines produces a discontinuity of the spectrum blueward of 3650°A. (the Balmer break) –more important in young populations, The break amplitude and position is a proxy for the age of th ...
... Classical indicators of what is going on: The limit of the Balmer series and the blending of the high-order Balmer lines produces a discontinuity of the spectrum blueward of 3650°A. (the Balmer break) –more important in young populations, The break amplitude and position is a proxy for the age of th ...
Chapter 11. Stellar Brightness, Magnitudes, the Distance
... 50 solar masses or perhaps a little larger. M-type stars have masses down below 0.1 solar masses. The smallest mass object that can start its nuclear fusion of Hydrogen is thought to be about 0.07 solar masses, so this represents the smallest stars we see. These are of class M. We do find cooler obj ...
... 50 solar masses or perhaps a little larger. M-type stars have masses down below 0.1 solar masses. The smallest mass object that can start its nuclear fusion of Hydrogen is thought to be about 0.07 solar masses, so this represents the smallest stars we see. These are of class M. We do find cooler obj ...
Sec 29.3 - Highland High School
... Internal pressure in white dwarfs A white dwarf is stable despite its lack of nuclear reactions because it is supported by the resistance of electrons being squeezed together. This pressure counteracts gravity and can support the core as long as the mass of the remaining core is less than about 1.4 ...
... Internal pressure in white dwarfs A white dwarf is stable despite its lack of nuclear reactions because it is supported by the resistance of electrons being squeezed together. This pressure counteracts gravity and can support the core as long as the mass of the remaining core is less than about 1.4 ...
13.1 Introduction 13.2 The Red Giant Branch
... outer layers of the star falls below ∼ 5000 K, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces the evolutionary track to travel almost vertically upwards to the red giant branch (RGB). The star now moves along the same path, ...
... outer layers of the star falls below ∼ 5000 K, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces the evolutionary track to travel almost vertically upwards to the red giant branch (RGB). The star now moves along the same path, ...
Lecture8
... The source function has units of intensity, Wm-3sr-1 As the ratio of two inverse processes (emission and absorption), the source function is relatively insensitive to the detailed properties of the stellar material. ...
... The source function has units of intensity, Wm-3sr-1 As the ratio of two inverse processes (emission and absorption), the source function is relatively insensitive to the detailed properties of the stellar material. ...
Cepheid variable stars
... What did Eddington mean when he said that a pulsating star can be characterised as a thermodynamic heat engine? Let’s consider layers inside the star as they expand and contract... ...
... What did Eddington mean when he said that a pulsating star can be characterised as a thermodynamic heat engine? Let’s consider layers inside the star as they expand and contract... ...
Abstract
... and find bright young objects there. Lyman α emitters1 have been recently discovered at redshifts greater than 3 (2.1109 yr after the Big-Bang) and Lyman break galaxies2 are high-redshift star-forming galaxies with the intense ultraviolet radiation from young stars. In the theoretical view point, g ...
... and find bright young objects there. Lyman α emitters1 have been recently discovered at redshifts greater than 3 (2.1109 yr after the Big-Bang) and Lyman break galaxies2 are high-redshift star-forming galaxies with the intense ultraviolet radiation from young stars. In the theoretical view point, g ...
Stellar Temperatures
... There is a great variety of stellar absorption lines; the strength of any individual line is determine by the star’s • Temperature (most important) • Gravity • Abundance Historically, stellar spectral types have been classified using letters; the temperature sequence is (hot-to-cool) O-B-A-F-G-K- ...
... There is a great variety of stellar absorption lines; the strength of any individual line is determine by the star’s • Temperature (most important) • Gravity • Abundance Historically, stellar spectral types have been classified using letters; the temperature sequence is (hot-to-cool) O-B-A-F-G-K- ...
stellar spectra instructor notes
... layers of all stars. Visible light penetrates not very deeply into stellar atmospheres, but goes deep enough to pass through the cool surface layers at the top of the atmospheres into deeper regions where the local temperatures are usually at least twice as high. Stellar atmospheres are therefore no ...
... layers of all stars. Visible light penetrates not very deeply into stellar atmospheres, but goes deep enough to pass through the cool surface layers at the top of the atmospheres into deeper regions where the local temperatures are usually at least twice as high. Stellar atmospheres are therefore no ...