Document
... Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted gas. Thus the iron abundances are artifically low, but the Carbon, ...
... Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted gas. Thus the iron abundances are artifically low, but the Carbon, ...
File
... star’s properties? • Challenges to using angular size – Due to distance, fuzzy images, even with telescopes – Large ground-based telescopes get better images, but the atmosphere blurs them some – Computer can de-blur it a little ...
... star’s properties? • Challenges to using angular size – Due to distance, fuzzy images, even with telescopes – Large ground-based telescopes get better images, but the atmosphere blurs them some – Computer can de-blur it a little ...
Document
... • The uncertainties in the f value is what limits you in practice. These depend on laboratory measurements, and for many lines poor values are known. • A differential analysis is usually employed. That is the ratio of abundances between stars (best if they have the same effective temperature). In th ...
... • The uncertainties in the f value is what limits you in practice. These depend on laboratory measurements, and for many lines poor values are known. • A differential analysis is usually employed. That is the ratio of abundances between stars (best if they have the same effective temperature). In th ...
a Supernova!
... Stellar material that started a little farther out falls in fractions of a second later, and rebounds off the now-dense core. This rebound is aided quite significantly by a momentary ‘overcontraction’of the neutron star core, which itself re-expands slightly and gives an extra outward ‘kick’ to the ...
... Stellar material that started a little farther out falls in fractions of a second later, and rebounds off the now-dense core. This rebound is aided quite significantly by a momentary ‘overcontraction’of the neutron star core, which itself re-expands slightly and gives an extra outward ‘kick’ to the ...
Module 6: “The Message of Starlight Assignment 9: Parallax, stellar
... Now, if we know the distance to the star, we can convert its brightness, measured in magnitudes (mag), to the magnitude a star would have at a fixed distance which has been chosen to be 10 parsecs, or about 32.6 light years. The equation we need is called the “distance modulus equation” and is a nic ...
... Now, if we know the distance to the star, we can convert its brightness, measured in magnitudes (mag), to the magnitude a star would have at a fixed distance which has been chosen to be 10 parsecs, or about 32.6 light years. The equation we need is called the “distance modulus equation” and is a nic ...
– 1 – 1. Cosmochronology
... The feature in the CMD usually used for age discrimination is the main sequence turnoff. The problem is that the turnoff is sensitive to heavy elements metallicity and to He content, as well as to age. An evaluation of an age depends on the validity of the full panoply of stellar evolution models, t ...
... The feature in the CMD usually used for age discrimination is the main sequence turnoff. The problem is that the turnoff is sensitive to heavy elements metallicity and to He content, as well as to age. An evaluation of an age depends on the validity of the full panoply of stellar evolution models, t ...
Lect07-2-4-09
... the orbital velocities of stars at different radii from the center. In such a model, we might have perfect circular orbits for stars in a perfectly flat disk in which the density of stars changes only with radius from the center and not with angle around the disk. We might also add a spherically dis ...
... the orbital velocities of stars at different radii from the center. In such a model, we might have perfect circular orbits for stars in a perfectly flat disk in which the density of stars changes only with radius from the center and not with angle around the disk. We might also add a spherically dis ...
test - Scioly.org
... 8. What does each dot on the H-R diagram represent? 9. What does the red line represent? 10. Mass, brightness, and temperature of main-sequence stars increase in which direction? 11. What spectral class is the star that is marked by the red “x”? 12. In the Yerkes classification scheme, stars are ass ...
... 8. What does each dot on the H-R diagram represent? 9. What does the red line represent? 10. Mass, brightness, and temperature of main-sequence stars increase in which direction? 11. What spectral class is the star that is marked by the red “x”? 12. In the Yerkes classification scheme, stars are ass ...
Galileo & the Telescope—Sept 21
... in a few days she was reduced to a semicircle. She maintained this shape for many days, all the while, however, growing in size. At present, she is becoming sickle-shaped… ...
... in a few days she was reduced to a semicircle. She maintained this shape for many days, all the while, however, growing in size. At present, she is becoming sickle-shaped… ...
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 ...
Lecture 17: Black Holes
... caused stars at high redshift to collapse to black holes, while present stars might be spared the same fate because of the lower densities and velocity dispersions in dark matter halos. The black holes formed at high redshift might account for some LMC microlensing events. • The model is so crazy th ...
... caused stars at high redshift to collapse to black holes, while present stars might be spared the same fate because of the lower densities and velocity dispersions in dark matter halos. The black holes formed at high redshift might account for some LMC microlensing events. • The model is so crazy th ...
Deriving the Isoradius Lines (optional, mathematical
... An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around the diagram. The options panel allows you to control the variables plotted on the x-axis: (temperature, BV, or spectral type) and those plotted on the y- ...
... An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around the diagram. The options panel allows you to control the variables plotted on the x-axis: (temperature, BV, or spectral type) and those plotted on the y- ...
August
... M13 At a distance of 25,100 light years, this globular cluster in the constellation Hercules (HER-cueleez) is about 145 light years in diameter. The age of M13 has been estimated at over 10 billion years. It contains over 300,000 stars. At the center, stars are about 500 times more concentrated than ...
... M13 At a distance of 25,100 light years, this globular cluster in the constellation Hercules (HER-cueleez) is about 145 light years in diameter. The age of M13 has been estimated at over 10 billion years. It contains over 300,000 stars. At the center, stars are about 500 times more concentrated than ...
Fulltext PDF - Indian Academy of Sciences
... their variety - while some are bright, some are faint; some are blue and red. The attempt to understand this vast variety eventually led to the physics of the structure of the stars. The brightness of a star is measured in magnitudes. Hipparchus, a Greek astronomer who lived a hundred and fifty year ...
... their variety - while some are bright, some are faint; some are blue and red. The attempt to understand this vast variety eventually led to the physics of the structure of the stars. The brightness of a star is measured in magnitudes. Hipparchus, a Greek astronomer who lived a hundred and fifty year ...
Slide 1
... Stellar Magnitude (brightness) Magnitude is the degree of brightness of a star. In 1856, British astronomer Norman Pogson proposed a quantitative scale of stellar magnitudes, which was adopted by the astronomical community. Each increment in magnitude corresponds to an increase in the amount of ene ...
... Stellar Magnitude (brightness) Magnitude is the degree of brightness of a star. In 1856, British astronomer Norman Pogson proposed a quantitative scale of stellar magnitudes, which was adopted by the astronomical community. Each increment in magnitude corresponds to an increase in the amount of ene ...
Crux The Southern Cross
... locked together gravitationally to form a binary star system. Sometimes double stars may only appear close together from our vantage point on earth. If in reality they do not interact then we call this an optical double. It is possible, but rarer for 4 or 6 stars to be grouped into Computer simulati ...
... locked together gravitationally to form a binary star system. Sometimes double stars may only appear close together from our vantage point on earth. If in reality they do not interact then we call this an optical double. It is possible, but rarer for 4 or 6 stars to be grouped into Computer simulati ...
Section 11: GRAPHIC STIMULUS
... In most large cities [6] like Singapore, we can only see a few of the large bright stars out in space. This is due to the increased pollution of earth [7] s atmosphere especially in the cities. The polluted skies obscure most of the other smaller stars [8] However [9] the stars are fascinating to so ...
... In most large cities [6] like Singapore, we can only see a few of the large bright stars out in space. This is due to the increased pollution of earth [7] s atmosphere especially in the cities. The polluted skies obscure most of the other smaller stars [8] However [9] the stars are fascinating to so ...
Black Holes & Quasars—18 Nov • Black hole • Quasar Ast 207 F2009
... waves are coincident with stars. • Stars do not emit light at radio wavelengths. • Are they some kind of weird star within the Milky Way Galaxy? Ast 207 F2009 ...
... waves are coincident with stars. • Stars do not emit light at radio wavelengths. • Are they some kind of weird star within the Milky Way Galaxy? Ast 207 F2009 ...
star a
... Main-sequence stars are stars like the Sun but with different masses. The mass-luminosity relation expresses a direct correlation between mass and luminosity for mainsequence stars. The greater the mass of a mainsequence star, the greater its luminosity (and also the greater its radius and surface t ...
... Main-sequence stars are stars like the Sun but with different masses. The mass-luminosity relation expresses a direct correlation between mass and luminosity for mainsequence stars. The greater the mass of a mainsequence star, the greater its luminosity (and also the greater its radius and surface t ...
Sample Final - IUPUI Physics
... D) nothing 48) Which of the following stars will undergo a supernova at the end of its lifetime? A) a star the mass of the sun B) a star at least 10 times the mass of the sun C) a star less than half the mass of the sun D) all of these stars will undergo a supernova at the end of their lifetimes 51) ...
... D) nothing 48) Which of the following stars will undergo a supernova at the end of its lifetime? A) a star the mass of the sun B) a star at least 10 times the mass of the sun C) a star less than half the mass of the sun D) all of these stars will undergo a supernova at the end of their lifetimes 51) ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.