1.2.43The stellar populations of the Milky Way
... main sequence stars burning hydrogen in their cores. The more massive stars that formed at the same time as the surviving low-mass ones have already left the main sequence and are now red giants or white dwarfs. For a long time it was thought that all Pop. II stars had much lower metallicities than ...
... main sequence stars burning hydrogen in their cores. The more massive stars that formed at the same time as the surviving low-mass ones have already left the main sequence and are now red giants or white dwarfs. For a long time it was thought that all Pop. II stars had much lower metallicities than ...
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... • RR Lyrae variables used like this to find our place in the Galaxy. • Distances that can be reached depend on the intrinsic brightness of the standard candle – and the limiting magnitude of your telescope ...
... • RR Lyrae variables used like this to find our place in the Galaxy. • Distances that can be reached depend on the intrinsic brightness of the standard candle – and the limiting magnitude of your telescope ...
TOOLS IN ASTRONOMY SPECTROSCOPY
... 2. Understand how stellar spectra are classified as A, B, C, D, E and so on, based on prominent characteristics. 3. Understand how stellar spectra are related to composition and temperature. Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can ...
... 2. Understand how stellar spectra are classified as A, B, C, D, E and so on, based on prominent characteristics. 3. Understand how stellar spectra are related to composition and temperature. Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can ...
12 Introduction to Cepheid Variable Stars Exercise
... The period of a cepheid variable ranges from 2.5 to 25 days compared to the day or less for an RR Lyrae. The period is the most significant characteristic that separates a cepheid variable from a RR Lyrae variable. The asymmetry of the light curve for a cepheid is similar to that of a RR Lyrae varia ...
... The period of a cepheid variable ranges from 2.5 to 25 days compared to the day or less for an RR Lyrae. The period is the most significant characteristic that separates a cepheid variable from a RR Lyrae variable. The asymmetry of the light curve for a cepheid is similar to that of a RR Lyrae varia ...
Fixed Stars
... Arcturus, it is not in the earthly catalog of starry astrological influences, for the time being. But the Creator God of this star seems to be very powerful on the Cosmic Mental Plane. The main influence here is from visiting or migrated humanlike intelligences from planets around Arcturus. Just as ...
... Arcturus, it is not in the earthly catalog of starry astrological influences, for the time being. But the Creator God of this star seems to be very powerful on the Cosmic Mental Plane. The main influence here is from visiting or migrated humanlike intelligences from planets around Arcturus. Just as ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... 1. Chapter 12, Question 1 in the text: To know certain properties of a star, you must first determine the star’s distance. For other properties, knowledge of distance is not necessary. Into which category would you place each of the following properties: size, mass, temperature, color, spectral type ...
... 1. Chapter 12, Question 1 in the text: To know certain properties of a star, you must first determine the star’s distance. For other properties, knowledge of distance is not necessary. Into which category would you place each of the following properties: size, mass, temperature, color, spectral type ...
Low mass stars
... Nearby stars: main-sequence appears. Most stars are less luminous and cooler than the Sun (alpha Centauri, nearest to us and a triple system, is similar). Note the hot small stars: the white dwarfs. ...
... Nearby stars: main-sequence appears. Most stars are less luminous and cooler than the Sun (alpha Centauri, nearest to us and a triple system, is similar). Note the hot small stars: the white dwarfs. ...
Observational properties of stars
... formulae so that they are only functions of density and temperature. So those boundaries mark locations where the dominant form of the gas transitions from one form to another. In reality you will not have exactly everything being in one form, there will tend to be some material that is in a slightl ...
... formulae so that they are only functions of density and temperature. So those boundaries mark locations where the dominant form of the gas transitions from one form to another. In reality you will not have exactly everything being in one form, there will tend to be some material that is in a slightl ...
The Origin, Structure, and Evolution of the Stars
... easy to show that the sun must convert four and a half million tons of matter into energy every second to maintain its present brightness. In the deep interior of the sun this would require more than 500 million tons of hydrogen converted to helium each second. The Evolution of Stars How long can th ...
... easy to show that the sun must convert four and a half million tons of matter into energy every second to maintain its present brightness. In the deep interior of the sun this would require more than 500 million tons of hydrogen converted to helium each second. The Evolution of Stars How long can th ...
Part 2 - Stellar Evolution
... core, causing the dormant core to contract The shell burning causes the outer envelope to expand and thus cooling, producing red giants The hydrogen shell burning occurs via the CNO cycle, the main source of N in the ...
... core, causing the dormant core to contract The shell burning causes the outer envelope to expand and thus cooling, producing red giants The hydrogen shell burning occurs via the CNO cycle, the main source of N in the ...
Presentation - Relativity Group
... • Spectral type is determined by a star’s surface temperature. • temperature dictates the energy states of electrons in atoms • temperature dictates the types of ions or molecules which exist • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • t ...
... • Spectral type is determined by a star’s surface temperature. • temperature dictates the energy states of electrons in atoms • temperature dictates the types of ions or molecules which exist • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • t ...
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... – L measures star’s “intrinsic” brightness, rather than “apparent” brightness seen from Earth ...
... – L measures star’s “intrinsic” brightness, rather than “apparent” brightness seen from Earth ...
12.748 Lecture 2 Cosmic Abundances, Nucleosynthesis and
... Here's a recipe for creating your own star: start with a "compressed" gas cloud, with as much as 1,000 atoms per cc of space1. Typically such cloud would be of order 3 to 4 x 1014 km across (that's 30-40 light years). This compression might be as a result of a collision between two galaxies or gas c ...
... Here's a recipe for creating your own star: start with a "compressed" gas cloud, with as much as 1,000 atoms per cc of space1. Typically such cloud would be of order 3 to 4 x 1014 km across (that's 30-40 light years). This compression might be as a result of a collision between two galaxies or gas c ...
No Slide Title
... 7. The nebulae around protostars are shaped into disks because of the same process that causes dough to become flat when it is a) spun in the air like pizza dough b) rolled with a pin like pizza dough c) squashed between plates like dough for a burrito d) baked on a flat sheet like a cookie. ...
... 7. The nebulae around protostars are shaped into disks because of the same process that causes dough to become flat when it is a) spun in the air like pizza dough b) rolled with a pin like pizza dough c) squashed between plates like dough for a burrito d) baked on a flat sheet like a cookie. ...
Studying Variable stars using Small Telescopes Observational
... Studying Variable stars using Small Telescopes Advantages of having Small Telescopes – 1. Convenient access to a telescope. 2. For sufficiently bright stars, small telescopes achieve same photometric accuracy as that of large telescopes. 3. With advanced increasing sophistications in optics and ele ...
... Studying Variable stars using Small Telescopes Advantages of having Small Telescopes – 1. Convenient access to a telescope. 2. For sufficiently bright stars, small telescopes achieve same photometric accuracy as that of large telescopes. 3. With advanced increasing sophistications in optics and ele ...
Stars - gilbertmath.com
... You have probably noticed, when looking at the sky at night, that some stars look as though they are grouped ____________________ into a distinct _____________________. Perhaps the best known star pattern in the northern hemisphere is the _________ ________________. ...
... You have probably noticed, when looking at the sky at night, that some stars look as though they are grouped ____________________ into a distinct _____________________. Perhaps the best known star pattern in the northern hemisphere is the _________ ________________. ...
the galaxy in which we live - Cosmos
... what we know as the Solar System. Our Solar System together with billions of other stars, planets, gas, dust, radiation, and invisible material (dark matter), are gravitationally bound forming a much larger structure: our Milky Way Galaxy. There are huge numbers of galaxies apart from our own, const ...
... what we know as the Solar System. Our Solar System together with billions of other stars, planets, gas, dust, radiation, and invisible material (dark matter), are gravitationally bound forming a much larger structure: our Milky Way Galaxy. There are huge numbers of galaxies apart from our own, const ...
Abundance of Elements
... I. Derive the stellar parameters of M dwarfs using the synthetic spectra in the long wavelength region of the optical spectra (over 8000 Å), which is relatively less contaminated by molecular lines as well as telluric lines. Test the synthetic spectrum for K2 III type star : HD 110014 ...
... I. Derive the stellar parameters of M dwarfs using the synthetic spectra in the long wavelength region of the optical spectra (over 8000 Å), which is relatively less contaminated by molecular lines as well as telluric lines. Test the synthetic spectrum for K2 III type star : HD 110014 ...
Introduction: The History and Technique of Stellar Classification
... von Fraunhofer early in the 1800’s, but it was not until late in that century that astronomers were able to routinely examine the spectra of stars in large numbers. Astronomers Angelo Secchi and E.C. Pickering were among the first to note that stellar spectra could be divided into groups by their ge ...
... von Fraunhofer early in the 1800’s, but it was not until late in that century that astronomers were able to routinely examine the spectra of stars in large numbers. Astronomers Angelo Secchi and E.C. Pickering were among the first to note that stellar spectra could be divided into groups by their ge ...
Additional Cosmology Images
... myriad of stars in crystal clear detail. The brilliant open star clusters are located about 200,000 lightyears away and are roughly 65 light-years across. Star clusters can be held together tightly by gravity, as is the case with densely packed crowds of hundreds of thousands of stars, called globul ...
... myriad of stars in crystal clear detail. The brilliant open star clusters are located about 200,000 lightyears away and are roughly 65 light-years across. Star clusters can be held together tightly by gravity, as is the case with densely packed crowds of hundreds of thousands of stars, called globul ...
Ch 11a (Measuring Stars 10-28-10)
... IV. Stellar sizes (radius) Luminosity is proportional to surface area (how large) x temperature (how hot): L= 4R2T4 If we can measure the Luminosity and the temperature of a star we can tell how large its ...
... IV. Stellar sizes (radius) Luminosity is proportional to surface area (how large) x temperature (how hot): L= 4R2T4 If we can measure the Luminosity and the temperature of a star we can tell how large its ...
PRS Questions (queestions after Midterm 2)
... lines (that are normally at visible wavelengths) are observed to be at ultraviolet wavelengths. Star B’s emission lines are observed to be at X-ray wavelengths. From these observations you conclude that: 1) both stars are moving away from the Earth 2) Star A is moving towards the Earth faster than S ...
... lines (that are normally at visible wavelengths) are observed to be at ultraviolet wavelengths. Star B’s emission lines are observed to be at X-ray wavelengths. From these observations you conclude that: 1) both stars are moving away from the Earth 2) Star A is moving towards the Earth faster than S ...
absolute brightness: The apparent brightness a star would have if it
... distance from the charge according to an inverse-square law. electromagnetic radiation: Consists of massless packets of pure energy called photons produced by changes in the energy of charged particles, usually electrons. Photons travel through space at the speed of light. When the changes of energy ...
... distance from the charge according to an inverse-square law. electromagnetic radiation: Consists of massless packets of pure energy called photons produced by changes in the energy of charged particles, usually electrons. Photons travel through space at the speed of light. When the changes of energy ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.