Stars, Galaxies, and the Universe
... Size, temperature (or color) and brightness Which is hotter-- a red star or a blue star? Why? Blue stars are hotter than red stars because gas glows red at lower temperatures and blue at higher temperatures. ...
... Size, temperature (or color) and brightness Which is hotter-- a red star or a blue star? Why? Blue stars are hotter than red stars because gas glows red at lower temperatures and blue at higher temperatures. ...
Lecture 8a Star Formation 10/15/2014
... Gravity and Star Formation Gravity causes the material (gas and dust) in a cloud to be attracted to each other • Compresses into smaller volume • Increases temperature and density • If the temperature at the center becomes large enough (5 million degrees) then H to He fusion can occur: • Star i ...
... Gravity and Star Formation Gravity causes the material (gas and dust) in a cloud to be attracted to each other • Compresses into smaller volume • Increases temperature and density • If the temperature at the center becomes large enough (5 million degrees) then H to He fusion can occur: • Star i ...
Pre-main sequence evolution
... i.e. its luminosity-temperature evolution, depends on the stellar mass. Solar-type stars develop radiative cores after the convective Hayashi phase. High-mass stars re-develop convective cores again during the radiatively-driven ...
... i.e. its luminosity-temperature evolution, depends on the stellar mass. Solar-type stars develop radiative cores after the convective Hayashi phase. High-mass stars re-develop convective cores again during the radiatively-driven ...
STAAR Science Tutorial 34 TEK 8.8A: Stars, Galaxies
... During the late 1800s and early 1900s, many scientists were using telescopes to catalog and classify all of the stars and other objects visible from Earth. Scientists noticed that there was great variation in the brightness and color of stars. Spectroscopes, which split white light into its componen ...
... During the late 1800s and early 1900s, many scientists were using telescopes to catalog and classify all of the stars and other objects visible from Earth. Scientists noticed that there was great variation in the brightness and color of stars. Spectroscopes, which split white light into its componen ...
STAAR Science Tutorial 28 TEK 8.8A: Stars
... During the late 1800s and early 1900s, many scientists were using telescopes to catalog and classify all of the stars and other objects visible from Earth. Scientists noticed that there was great variation in the brightness and color of stars. Spectroscopes, which split white light into its componen ...
... During the late 1800s and early 1900s, many scientists were using telescopes to catalog and classify all of the stars and other objects visible from Earth. Scientists noticed that there was great variation in the brightness and color of stars. Spectroscopes, which split white light into its componen ...
18. Formation of Stars.
... like the Sun, it will remain on the Main Sequence for about 10 billion yrs. • While on the Main Sequence, stars are in pressure equilibrium. That is, there is a balance between the force of gravity (directed toward the star's center) and thermal (or heat) pressure caused by energy released from t ...
... like the Sun, it will remain on the Main Sequence for about 10 billion yrs. • While on the Main Sequence, stars are in pressure equilibrium. That is, there is a balance between the force of gravity (directed toward the star's center) and thermal (or heat) pressure caused by energy released from t ...
Biography of a Star - Max-Planck
... process. At the same time, however, the outer shell greatly expands, causing the surface temperature to fall from values of some 6,000 degrees to around 3,000 degrees Celsius. The Sun has increased its radius a hundredfold, and shines with a reddish light up to 5,000 times as brightly as it does at ...
... process. At the same time, however, the outer shell greatly expands, causing the surface temperature to fall from values of some 6,000 degrees to around 3,000 degrees Celsius. The Sun has increased its radius a hundredfold, and shines with a reddish light up to 5,000 times as brightly as it does at ...
T Tauri Stars
... Are winds originating in disks or is there another explanation for this correlation What are the transport mechanisms for mass infall? Why are CTTSs so aperiodic? What causes the massive flaring of FU Orionis outbursts? ...
... Are winds originating in disks or is there another explanation for this correlation What are the transport mechanisms for mass infall? Why are CTTSs so aperiodic? What causes the massive flaring of FU Orionis outbursts? ...
Photometry
... measured for other pairs of filters. • The U-B measurement brackets the Balmer line at 364 nm. – Opaque at shorter wavelength • This creates a discontinuity in energy measurement. – Greatest at type A – Drop off for B and G ...
... measured for other pairs of filters. • The U-B measurement brackets the Balmer line at 364 nm. – Opaque at shorter wavelength • This creates a discontinuity in energy measurement. – Greatest at type A – Drop off for B and G ...
giants1
... •The youngest stars (age < 1 gyrs, 17.1 stars) are compatible with a single value of [Fe/H] (sigma=0.09). • Spread become significant at higher ages; at 4 Gyrs much larger than measurement errors. ...
... •The youngest stars (age < 1 gyrs, 17.1 stars) are compatible with a single value of [Fe/H] (sigma=0.09). • Spread become significant at higher ages; at 4 Gyrs much larger than measurement errors. ...
27B Star Life Cycle and the HR Diagram
... Just like humans, stars go through a life cycle. Over the course of their lives, stars change in ways that make each stage different and recognizable. A useful way to organize this information is in a Hertzsprung-Russell diagram, also called an H-R diagram. In this investigation, you will learn how ...
... Just like humans, stars go through a life cycle. Over the course of their lives, stars change in ways that make each stage different and recognizable. A useful way to organize this information is in a Hertzsprung-Russell diagram, also called an H-R diagram. In this investigation, you will learn how ...
A star is born: understanding the physics of star formation
... These molecular clouds can be in an approximate equilibrium between the forces acting to expand the cloud and those trying to collapse it (primarily gravity). However, if this equilibrium is perturbed, either by an external force, such as a supernova explosion, or by the cloud becoming sufficiently ...
... These molecular clouds can be in an approximate equilibrium between the forces acting to expand the cloud and those trying to collapse it (primarily gravity). However, if this equilibrium is perturbed, either by an external force, such as a supernova explosion, or by the cloud becoming sufficiently ...
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
... The data in Fig 2 constitute a straight line in the classes O5 – F0 and F6 – K5 in accordance with the usual HRdiagram. In equation 3 hνmax = 1.6 θ, where θ = internal electron temperature in eV. This means that the classes O5 – F0 have higher temperature than the classes F6 – K5, which is also in a ...
... The data in Fig 2 constitute a straight line in the classes O5 – F0 and F6 – K5 in accordance with the usual HRdiagram. In equation 3 hνmax = 1.6 θ, where θ = internal electron temperature in eV. This means that the classes O5 – F0 have higher temperature than the classes F6 – K5, which is also in a ...
Lecture 3 Radiative and Convective Energy Transport I
... In a star the heat flux must be sufficiently great to transport all the energy that is liberated. This requires a temperature gradient. The higher the energy flux, the larger the temperature gradient. But the temperature gradient cannot increase without limits. At some point instability sets in and ...
... In a star the heat flux must be sufficiently great to transport all the energy that is liberated. This requires a temperature gradient. The higher the energy flux, the larger the temperature gradient. But the temperature gradient cannot increase without limits. At some point instability sets in and ...
Goal: To understand the HR diagram
... • At different temperatures, the blackbody spectrum peaks out at a different part of the spectrum. • Hot stars peak in the blue – so they appear to be blue. • Moderate stars peak in the middle, so appear to be yellow to white. • Cooler stars peak in the red, so appear to be orange to red. ...
... • At different temperatures, the blackbody spectrum peaks out at a different part of the spectrum. • Hot stars peak in the blue – so they appear to be blue. • Moderate stars peak in the middle, so appear to be yellow to white. • Cooler stars peak in the red, so appear to be orange to red. ...
Poster - Arkansas Center for Space and Planetary Sciences
... and blocking some of the light. GX Gem belongs to a category of binary stars called close binaries since the two stars cannot be individually resolved in a telescope. By studying the variation in light in images taken from November 2001 to April 2006, the properties of the stars as well as of the or ...
... and blocking some of the light. GX Gem belongs to a category of binary stars called close binaries since the two stars cannot be individually resolved in a telescope. By studying the variation in light in images taken from November 2001 to April 2006, the properties of the stars as well as of the or ...
Spatial Structure Evolution of Star Clusters
... - Full data release expected end of 2002 - Deep IR images to differentiate the MS (IR camera with Nagoya U & PMO) • Stars in an open cluster, regardless of masses, are concentrated progressively toward the center. • The youngest star clusters show evidence of luminosity (mass) segregation - cf. mole ...
... - Full data release expected end of 2002 - Deep IR images to differentiate the MS (IR camera with Nagoya U & PMO) • Stars in an open cluster, regardless of masses, are concentrated progressively toward the center. • The youngest star clusters show evidence of luminosity (mass) segregation - cf. mole ...
Stars: Part 2
... • It is brighter than 10 billion stars put together. • A supernova can even be SO bright that it outshines an entire galaxy for a few seconds. • More than 90% of a star’s mass is blown away in this explosion. • Heavier elements like gold and uranium are made as the atomic nuclei are smashed together ...
... • It is brighter than 10 billion stars put together. • A supernova can even be SO bright that it outshines an entire galaxy for a few seconds. • More than 90% of a star’s mass is blown away in this explosion. • Heavier elements like gold and uranium are made as the atomic nuclei are smashed together ...
Blackbody radiation Temperature of stars
... Transparent for everything: no color Absorbs everything, but yellow: yellow Absorbs everything, but red: red ...
... Transparent for everything: no color Absorbs everything, but yellow: yellow Absorbs everything, but red: red ...
Stellar evolution - Chandra X
... where gas has been heated to very high temperatures or particles have been accelerated to extremely high energies. These conditions can exist near collapsed objects such as white dwarfs, neutron stars, and black holes; in giant bubbles of hot gas produced by supernovas; in stellar winds; or in the h ...
... where gas has been heated to very high temperatures or particles have been accelerated to extremely high energies. These conditions can exist near collapsed objects such as white dwarfs, neutron stars, and black holes; in giant bubbles of hot gas produced by supernovas; in stellar winds; or in the h ...
Lectures 12 & 13 powerpoint (stellar death)
... Q: The Helium core contracts and heats the star enough to induce a hydrogen-burning shell… so what stops the helium core from contracting to zero radius (keep in mind that He fusion has not set in yet….)? A: Degeneracy pressure! The core becomes very dense… and two laws of quantum mechanics becom ...
... Q: The Helium core contracts and heats the star enough to induce a hydrogen-burning shell… so what stops the helium core from contracting to zero radius (keep in mind that He fusion has not set in yet….)? A: Degeneracy pressure! The core becomes very dense… and two laws of quantum mechanics becom ...
Life Cycle of a Star - Intervention Worksheet
... All stars start as a nebula. A nebula is a large cloud of gas and dust. Gravity can pull some of the gas and dust in a nebula together. The contracting cloud is then called a protostar. A protostar is the earliest stage of a star’s life. A star is born when the gas and dust from a nebula become so h ...
... All stars start as a nebula. A nebula is a large cloud of gas and dust. Gravity can pull some of the gas and dust in a nebula together. The contracting cloud is then called a protostar. A protostar is the earliest stage of a star’s life. A star is born when the gas and dust from a nebula become so h ...
Equation of state constraints for the cold dense matter inside neutron
... J1810.8-260. Care is taken to use only the hard state bursts where it is thought that the NS surface alone is emitting. We then use a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius ...
... J1810.8-260. Care is taken to use only the hard state bursts where it is thought that the NS surface alone is emitting. We then use a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius ...
Astrophysics
... a. (2 pts) Write or derive an equation for hydrostatic equilibrium in a form that is suitable for the interior of the sun, i.e., express dP/dr in terms of G, m, ρ, and r, where m is the mass interior to radius r and ρ is the mass density. b. (1 pt) Rewrite the equation with m as the independent vari ...
... a. (2 pts) Write or derive an equation for hydrostatic equilibrium in a form that is suitable for the interior of the sun, i.e., express dP/dr in terms of G, m, ρ, and r, where m is the mass interior to radius r and ρ is the mass density. b. (1 pt) Rewrite the equation with m as the independent vari ...
Main-sequence stage Stellar lifetimes
... Mass Luminosity Main-sequence time (M) (L) (106 years) ...
... Mass Luminosity Main-sequence time (M) (L) (106 years) ...