Abundance of Elements
... Synthetic spectra for cool stars were retrieved from the website of the PHOENIX project( http://www.hs.unihamburg.de/EN/For/ThA/phoenix) critical metallicity calibration has now been initiated based on atmospheric modeling of Fe lines using high resolution spectra of bright (mostly early-type)M ...
... Synthetic spectra for cool stars were retrieved from the website of the PHOENIX project( http://www.hs.unihamburg.de/EN/For/ThA/phoenix) critical metallicity calibration has now been initiated based on atmospheric modeling of Fe lines using high resolution spectra of bright (mostly early-type)M ...
NATS1311_112008_bw
... • We finally obtained direct evidence of the existence of an extrasolar planet in the year 1995. – A planet was discovered in orbit around the star 51 Pegasi. – Over 200 such extrasolar planets are now known to exist. ...
... • We finally obtained direct evidence of the existence of an extrasolar planet in the year 1995. – A planet was discovered in orbit around the star 51 Pegasi. – Over 200 such extrasolar planets are now known to exist. ...
More detailed notes - Particle Physics and Particle Astrophysics
... the Sun is a slowly contracting pre-mainsequence star. Its surface temperature is just under 4000 K, but it is very large, so it’s substantially more luminous than it will be on the main sequence. 2. As contraction proceeds, the young star initially remains at about the same surface temperature, but ...
... the Sun is a slowly contracting pre-mainsequence star. Its surface temperature is just under 4000 K, but it is very large, so it’s substantially more luminous than it will be on the main sequence. 2. As contraction proceeds, the young star initially remains at about the same surface temperature, but ...
Name - MIT
... 39) The two most abundant elements in the Earth’s atmosphere are … A) hydrogen and helium. B) iron and hydrogen. C) nitrogen and hydrogen. D) oxygen and carbon. E) nitrogen and oxygen. 40) Half-life is defined as … A) The age of the solar system B) The age of the universe C) The time required for ha ...
... 39) The two most abundant elements in the Earth’s atmosphere are … A) hydrogen and helium. B) iron and hydrogen. C) nitrogen and hydrogen. D) oxygen and carbon. E) nitrogen and oxygen. 40) Half-life is defined as … A) The age of the solar system B) The age of the universe C) The time required for ha ...
ph507lecnote06
... obtained quantities. Important stars: no obvious pattern…Sirius B, Betelgeus in opposite corners: ...
... obtained quantities. Important stars: no obvious pattern…Sirius B, Betelgeus in opposite corners: ...
Star
... Where do we come from? • The first (and simplest) atoms were created during the Big Bang. • More complex atoms were created in stars. • When the star dies, they are expelled into space…. to form new stars and planets! Most of the atoms in our bodies were created in the core of a star! ...
... Where do we come from? • The first (and simplest) atoms were created during the Big Bang. • More complex atoms were created in stars. • When the star dies, they are expelled into space…. to form new stars and planets! Most of the atoms in our bodies were created in the core of a star! ...
BrainPOP - The Science Spot
... 4. A red giant star has a _____________ that has cooled and glows red. It burns helium and fuses it into heavier _____________. Since these reactions are not as powerful as burning hydrogen, the star starts to _____________ after about 10 __________ years. 5. What happens after this point depends on ...
... 4. A red giant star has a _____________ that has cooled and glows red. It burns helium and fuses it into heavier _____________. Since these reactions are not as powerful as burning hydrogen, the star starts to _____________ after about 10 __________ years. 5. What happens after this point depends on ...
Interstellar medium, birth and life of stars
... How will our Sun evolve as a star? What will its final state be? Compare its predicted evolution to that of higher-mass stars. How do they end? How do we know? ...
... How will our Sun evolve as a star? What will its final state be? Compare its predicted evolution to that of higher-mass stars. How do they end? How do we know? ...
4550-15Lecture33
... helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship between the main sequence lifetime of a star and mass. The most massive stars, up to ~100 solar ma ...
... helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship between the main sequence lifetime of a star and mass. The most massive stars, up to ~100 solar ma ...
Galaxies
... central bulge • Forms spiral arms that contain a lot of gas and dust • Population I stars are found in the spiral arms – these are young O and B main-sequence stars – they are often found in open clusters ...
... central bulge • Forms spiral arms that contain a lot of gas and dust • Population I stars are found in the spiral arms – these are young O and B main-sequence stars – they are often found in open clusters ...
Part 1—Stages of Human Life
... 1. Make an educated guess of the life cycle of the images of the stars. Guess the stages of life for this high mass star. 2. Shuffle the images and place them in order from youngest to oldest, but do NOT glue them down yet. 3. List the logic and the reasons for why you placed the images in the order ...
... 1. Make an educated guess of the life cycle of the images of the stars. Guess the stages of life for this high mass star. 2. Shuffle the images and place them in order from youngest to oldest, but do NOT glue them down yet. 3. List the logic and the reasons for why you placed the images in the order ...
Chapter 19 Star Formation
... “distorted way: In fact the clouds are usually much more irregular than shown in this textbook illustration. (Note: all the colorful emission line nebulae shown in this chapter are just this same molecular gas after a massive stars has started pouring out photons. ...
... “distorted way: In fact the clouds are usually much more irregular than shown in this textbook illustration. (Note: all the colorful emission line nebulae shown in this chapter are just this same molecular gas after a massive stars has started pouring out photons. ...
Planets
... objects in space pass by the twinkling stars and slowly travel across the sky. Moving space objects are usually planets. The word planet comes from the Greek word ...
... objects in space pass by the twinkling stars and slowly travel across the sky. Moving space objects are usually planets. The word planet comes from the Greek word ...
Telescopes
... Twinkling of Stars • Air bends (refracts) starlight. Due to the atmospheric turbulence, the bending varies with time, so the amount of light hitting your eyes varies. • Stars closer to the horizon => more air, more turbulence => more twinkling! • This causes blurring of the star’s image, so that it ...
... Twinkling of Stars • Air bends (refracts) starlight. Due to the atmospheric turbulence, the bending varies with time, so the amount of light hitting your eyes varies. • Stars closer to the horizon => more air, more turbulence => more twinkling! • This causes blurring of the star’s image, so that it ...
Fulltext PDF - Indian Academy of Sciences
... them the music of the spheres 13, attributing specific notes to the various planets. He said that there was no audible sound there but that “the movements of the planets are modulated according to harmonic proportions.” By his painstaking analysis of the data on the orbit of Mars, which had been col ...
... them the music of the spheres 13, attributing specific notes to the various planets. He said that there was no audible sound there but that “the movements of the planets are modulated according to harmonic proportions.” By his painstaking analysis of the data on the orbit of Mars, which had been col ...
Scattering (and the blue sky)
... In other galaxies, the arms are easy to see because their ISM does not hide optical diagnostics from us. There are always only a few arms (often 2), and they are never too tightly wound. O & B stars ...
... In other galaxies, the arms are easy to see because their ISM does not hide optical diagnostics from us. There are always only a few arms (often 2), and they are never too tightly wound. O & B stars ...
A NEW FAMILY OF PLANETS? “OCEAN
... measurements so that their radius and mass can be determined simultaneously. Their composition is, in mass, 50% rocks and metals, 50% ices, as can be expected from the disc chemical composition; 2. the initial composition of ices is similar to that of comets, mostly H2O and some NH3 and CO2 . To sim ...
... measurements so that their radius and mass can be determined simultaneously. Their composition is, in mass, 50% rocks and metals, 50% ices, as can be expected from the disc chemical composition; 2. the initial composition of ices is similar to that of comets, mostly H2O and some NH3 and CO2 . To sim ...
Foundation 1 - Discovering Astronomy
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just outsid ...
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just outsid ...
May - RASC St. John`s Centre
... Square of Pegasus, The Winged Horse, 35º away. All of the very bright stars mentioned above, along with many of the other brighter ones in each constellation, are more obvious and easier to locate during twilight, before all the fainter stars surrounding them become visible as well. These won’t all ...
... Square of Pegasus, The Winged Horse, 35º away. All of the very bright stars mentioned above, along with many of the other brighter ones in each constellation, are more obvious and easier to locate during twilight, before all the fainter stars surrounding them become visible as well. These won’t all ...
Stellar Evolution
... Star of more than 8 solar masses can fuse elements far beyond carbon in its core Leads to a very different fate Path across the H-R diagram is essentially a straight line Stays at just about the same luminosity as it cools off Eventually the star dies in a violent explosion called a supernova ...
... Star of more than 8 solar masses can fuse elements far beyond carbon in its core Leads to a very different fate Path across the H-R diagram is essentially a straight line Stays at just about the same luminosity as it cools off Eventually the star dies in a violent explosion called a supernova ...
William Paterson University Department of Physics General
... Every student at William Paterson has a student university e-mail address. Your university email address is attached to Blackboard, and that is the one that will be used to contact you about assignments and other matters related to the course. You should check it daily. AOL users: if you have AOL, y ...
... Every student at William Paterson has a student university e-mail address. Your university email address is attached to Blackboard, and that is the one that will be used to contact you about assignments and other matters related to the course. You should check it daily. AOL users: if you have AOL, y ...
A method to get objective spectra of exoplanets
... 2) National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 Abstract The main problem in the direct detection of exoplanets is the suppression of starlight. A high-contrast imaging scheme must be realized for the detection of faint companions. Several kinds of differential me ...
... 2) National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 Abstract The main problem in the direct detection of exoplanets is the suppression of starlight. A high-contrast imaging scheme must be realized for the detection of faint companions. Several kinds of differential me ...
