Stellar Evolution
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
9 spectroscopic parallax
... Absolute magnitude = how bright (what magnitude) a star would appear at 10 parsecs (32.6 light years) ...
... Absolute magnitude = how bright (what magnitude) a star would appear at 10 parsecs (32.6 light years) ...
The Big Dipper Constellation
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
... The Big Dipper What is a Constellation? From very early times, man has been fascinated by the stars. Early stargazers began naming stars. They also noticed patterns of stars that appeared night after night in the sky. These patterns or groupings of stars are called constellations. They also began to ...
Lecture 29 Our Galaxy: "Milky Way"
... Galactic Rotation Galactic material must be in some kind of orbit around the center, or gravity would pull everything into the center! • Rotation of Galaxy is real tough to measure (can't actually see rotation in our lifetime), but get a rough idea as follows, mainly from doppler radial velocities: ...
... Galactic Rotation Galactic material must be in some kind of orbit around the center, or gravity would pull everything into the center! • Rotation of Galaxy is real tough to measure (can't actually see rotation in our lifetime), but get a rough idea as follows, mainly from doppler radial velocities: ...
Low mass stars
... from the hot core left behind. The White Dwarf core has a surface temperature over 100,000 K. Wein's law for a hot body with this temperature gives a peak wavelength of 2.9 x 10 -8m, corresponding to ultraviolet light. When the electrons recombine with the surrounding ions, they often enter an excit ...
... from the hot core left behind. The White Dwarf core has a surface temperature over 100,000 K. Wein's law for a hot body with this temperature gives a peak wavelength of 2.9 x 10 -8m, corresponding to ultraviolet light. When the electrons recombine with the surrounding ions, they often enter an excit ...
Gilmore
... Implications for/from Astrophysics: Can one plausibly build a dSph as observed without disturbing the DM? Star formation histories and IMF are easily determined survival history, energy input… Chemical element distributions define gas flows, accretion/wind rates, debris from destruction make ...
... Implications for/from Astrophysics: Can one plausibly build a dSph as observed without disturbing the DM? Star formation histories and IMF are easily determined survival history, energy input… Chemical element distributions define gas flows, accretion/wind rates, debris from destruction make ...
Stars, Galaxies, and the Universe Section 1 Section 1
... from Earth, is caused by the movement of Earth. • The stars seem as though they are moving counterclockwise around a central star called Polaris, the North Star. Polaris is almost directly above the North Pole, and thus the star does not appear to move much. • Earth’s revolution around the sun cause ...
... from Earth, is caused by the movement of Earth. • The stars seem as though they are moving counterclockwise around a central star called Polaris, the North Star. Polaris is almost directly above the North Pole, and thus the star does not appear to move much. • Earth’s revolution around the sun cause ...
light
... the aid of new observations of Blanco 1, an high-Galactic latitude, Pleiades-age cluster, I will show how deriving stellar age must be based upon very high quality observational data and a diverse range of stellar models. ...
... the aid of new observations of Blanco 1, an high-Galactic latitude, Pleiades-age cluster, I will show how deriving stellar age must be based upon very high quality observational data and a diverse range of stellar models. ...
Spectroscopy PPT
... element has its own unique line spectrum, like a fingerprint) 2. Tells us if galaxies and stars are moving away from us or toward us (called?) ...
... element has its own unique line spectrum, like a fingerprint) 2. Tells us if galaxies and stars are moving away from us or toward us (called?) ...
Spectra of Star Clusters
... stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, d ...
... stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, d ...
Slide 1
... helium. At these temperatures most of the hydrogen is ionized, so the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. ...
... helium. At these temperatures most of the hydrogen is ionized, so the hydrogen lines are weak. Both HeI and HeII (singly ionized helium) are seen in the higher temperature examples. The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across. ...
Chapter 6: Stellar Evolution (part 2)
... The hotter a star’s core becomes, the higher energy the gamma rays it produces. When the mass of a star exceeds about 100M , the produced gamma rays become so energetic, their interaction with atomic nucleus can lead to the production of electron-position pairs. The pair production decreases the di ...
... The hotter a star’s core becomes, the higher energy the gamma rays it produces. When the mass of a star exceeds about 100M , the produced gamma rays become so energetic, their interaction with atomic nucleus can lead to the production of electron-position pairs. The pair production decreases the di ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... Nebulae and White Dwarfs are in order. – The shell of gas that is visible in each planetary nebula illustrates that stars have a way of returning material to the interstellar medium that has undergone nuclear processing. – Over time, the hot “central star” of a PN cools to become a white dwarf: • Ap ...
... Nebulae and White Dwarfs are in order. – The shell of gas that is visible in each planetary nebula illustrates that stars have a way of returning material to the interstellar medium that has undergone nuclear processing. – Over time, the hot “central star” of a PN cools to become a white dwarf: • Ap ...
Acceleration of Coronal Mass Ejection In Long Rising Solar
... Four stages of star formation 1. Form proto-star core within molecular cloud 2. Core grows from surrounding rotating disk 3. Bipolar flow along rotation axis 4. New star clears away the surrounding nebular material ...
... Four stages of star formation 1. Form proto-star core within molecular cloud 2. Core grows from surrounding rotating disk 3. Bipolar flow along rotation axis 4. New star clears away the surrounding nebular material ...
Document
... Stars as Black Bodies? Thermal Equilibrium? Basic condition for the BB as emitting source negligible fraction of radiation escapes! Below the lower photosphere optical depth to the surface is high enough to prevent escape of most photons. They are reabsorbed close to where they were emitted therm ...
... Stars as Black Bodies? Thermal Equilibrium? Basic condition for the BB as emitting source negligible fraction of radiation escapes! Below the lower photosphere optical depth to the surface is high enough to prevent escape of most photons. They are reabsorbed close to where they were emitted therm ...
• This chapter concentrates on five goals:
... • As you have learned, hydrogen Balmer absorption lines are produced by hydrogen atoms with electrons initially in the second energy level. It takes a specific amount of energy to get an electron from one energy Level to another ...
... • As you have learned, hydrogen Balmer absorption lines are produced by hydrogen atoms with electrons initially in the second energy level. It takes a specific amount of energy to get an electron from one energy Level to another ...
Stellar Structure - McMurry University
... A. The temperature at their centers never gets high enough. B. The density at their centers is too low. C. Iron fusion consumes energy. D. Not enough iron is present. ...
... A. The temperature at their centers never gets high enough. B. The density at their centers is too low. C. Iron fusion consumes energy. D. Not enough iron is present. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.