How Bright is that Star?
... A 1st magnitude star is 100x brighter than a “6th ” Each order of magnitude is therefore 2.15 times brighter than the one below it. Magnitude is now given in decimal form. Deneb now rates a 1.26, and Betelgeuse rates .87. Hipparchus underestimated how bright the brightest were, so now we even use ne ...
... A 1st magnitude star is 100x brighter than a “6th ” Each order of magnitude is therefore 2.15 times brighter than the one below it. Magnitude is now given in decimal form. Deneb now rates a 1.26, and Betelgeuse rates .87. Hipparchus underestimated how bright the brightest were, so now we even use ne ...
Outline - Picnic Point High School
... The Universe began with a singularity in space-time. After the initial explosion, the Universe started to expand, cool and condense, forming matter. As part of this ongoing process the Sun and the Solar System were formed over 4x109 years ago from a gas cloud which resulted from a supernova explosio ...
... The Universe began with a singularity in space-time. After the initial explosion, the Universe started to expand, cool and condense, forming matter. As part of this ongoing process the Sun and the Solar System were formed over 4x109 years ago from a gas cloud which resulted from a supernova explosio ...
Nonlinear Tides in Exoplanet Host Stars - CIERA
... • Accurate theories of tidal dissipation are needed to understand and make predictions for orbit/spin evolution. • The guilty pleasure of constant Q. •The linear tide gives very long orbital decay times, and ...
... • Accurate theories of tidal dissipation are needed to understand and make predictions for orbit/spin evolution. • The guilty pleasure of constant Q. •The linear tide gives very long orbital decay times, and ...
The Milky Way - Montgomery College
... Strategies to explore the structure of our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances. II. Observe objects at wavelengths other than visible (to circumvent the problem of optical obscuration), and catalog their directions an ...
... Strategies to explore the structure of our Milky Way I. Select bright objects that you can see throughout the Milky Way and trace their directions and distances. II. Observe objects at wavelengths other than visible (to circumvent the problem of optical obscuration), and catalog their directions an ...
Stellar Nebulae
... galaxies, reaching up to 300 light years in diameter. They contain enough dense gas and dust to form hundreds of thousands of Sun-like stars. These stars are formed in the densest parts of the clouds. Molecular clouds are very cold, having temperatures ranging from about -440 to -370 degrees Fahrenh ...
... galaxies, reaching up to 300 light years in diameter. They contain enough dense gas and dust to form hundreds of thousands of Sun-like stars. These stars are formed in the densest parts of the clouds. Molecular clouds are very cold, having temperatures ranging from about -440 to -370 degrees Fahrenh ...
Answers to Odd-Numbered Exercises and Problems
... c. The gravitational force on the solar system is the net force due to all the matter inside our orbit. Most of that matter is concentrated near the center of the galaxy. Assume that the matter has a spherical distribution, like a giant star. What is the approximate mass of the galactic center? d. A ...
... c. The gravitational force on the solar system is the net force due to all the matter inside our orbit. Most of that matter is concentrated near the center of the galaxy. Assume that the matter has a spherical distribution, like a giant star. What is the approximate mass of the galactic center? d. A ...
What would the sky look like from the North Pole
... d) Saturn is presently at a distance of about 10 AU from the Earth. How long does it take a radio signal from the Cassini spacecraft to reach the mission control center in California? Radio waves travel at the speed of light, which is 3 x 105 km/s. 1 AU is 1.5 x 108 km. ...
... d) Saturn is presently at a distance of about 10 AU from the Earth. How long does it take a radio signal from the Cassini spacecraft to reach the mission control center in California? Radio waves travel at the speed of light, which is 3 x 105 km/s. 1 AU is 1.5 x 108 km. ...
Type Ia Supernovae as distance indicators
... • Peak magnitude variation: ~0.3 • Much of this can be corrected for ...
... • Peak magnitude variation: ~0.3 • Much of this can be corrected for ...
star-formation rate
... e.g., massive stars leave the main sequence after several 106 years, the number of luminous blue stars thus decreases, so the spectral distribution of the population also changes in time. • The spectral energy distribution (SED) of a galaxy reflects its history of star formation and stellar evolutio ...
... e.g., massive stars leave the main sequence after several 106 years, the number of luminous blue stars thus decreases, so the spectral distribution of the population also changes in time. • The spectral energy distribution (SED) of a galaxy reflects its history of star formation and stellar evolutio ...
Galactic Evolution:
... times in the Milky Way with the same metallicity as the Sun will not necessarily form habitable Earth like planets. As a result of the radial Galactic metafficity gradient, the outer limit of the GHZ is set primarily by the minimum required metallicity to build large terrestrial planets. Regions of ...
... times in the Milky Way with the same metallicity as the Sun will not necessarily form habitable Earth like planets. As a result of the radial Galactic metafficity gradient, the outer limit of the GHZ is set primarily by the minimum required metallicity to build large terrestrial planets. Regions of ...
Stars, Galaxies, and the Universe Section 1 Distances to Stars
... • Stars vary in size and mass. • Stars such as the sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less mas ...
... • Stars vary in size and mass. • Stars such as the sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. • Most of the stars you can see in the night sky are medium-sized stars. • Many stars also have about the same mass as the sun, however some stars may be more or less mas ...
Homework No. 2 Solutions
... section of the Vega spectrum in black. You may assume that Vega is not moving. The red plot is part of the spectrum from another star very similar to Vega except for its Doppler shift. The numbers show the location of the spectral line. You will find It helpful to ...
... section of the Vega spectrum in black. You may assume that Vega is not moving. The red plot is part of the spectrum from another star very similar to Vega except for its Doppler shift. The numbers show the location of the spectral line. You will find It helpful to ...
Where to begin the adventure with variable stars?
... In this way we have found the stars and we can begin photometric observations. Their result will probably impress not only us, but also other students and our friends. Also the acquired skills of navigating in the sky will be a source of satisfaction! ...
... In this way we have found the stars and we can begin photometric observations. Their result will probably impress not only us, but also other students and our friends. Also the acquired skills of navigating in the sky will be a source of satisfaction! ...
PPT - Yale University
... mechanisms depend in some way on external circumstances (e.g. ionization). A very large disk is needed and transport times are very long (103 to 106 rotation periods) because disks are fragile and cannot sustain a large torque. Most disks probably do not last this long before being disrupted by ...
... mechanisms depend in some way on external circumstances (e.g. ionization). A very large disk is needed and transport times are very long (103 to 106 rotation periods) because disks are fragile and cannot sustain a large torque. Most disks probably do not last this long before being disrupted by ...
Globular Clusters - Lick Observatory
... University of California Observatories - Lick Observatories, Elinor Gates ...
... University of California Observatories - Lick Observatories, Elinor Gates ...
GEK - National University of Singapore
... b) What are the advantages and (c) disadvantages of this technique? It’s arguably the most straightforward and simplest measurement technique… well, except that it only works for relatively nearby stars >_< ...
... b) What are the advantages and (c) disadvantages of this technique? It’s arguably the most straightforward and simplest measurement technique… well, except that it only works for relatively nearby stars >_< ...
The Abundances of the Fe Group Elements in Three Early B Stars in
... Geraldine J. Peters Space Sciences Center/Dept. of Physics & Astronomy University of Southern California Los Angeles, CA 90089-1341 ...
... Geraldine J. Peters Space Sciences Center/Dept. of Physics & Astronomy University of Southern California Los Angeles, CA 90089-1341 ...
– 1 – 1. Cosmochronology
... specific star if the lifetime of the decaying isotope is known (that is usually well known from lab measurements), if the initial abundance of the decaying isotope is known, and if the current isotopic abundance, or the abundance of the product of the decay (sometimes called the “daughter”), can be ...
... specific star if the lifetime of the decaying isotope is known (that is usually well known from lab measurements), if the initial abundance of the decaying isotope is known, and if the current isotopic abundance, or the abundance of the product of the decay (sometimes called the “daughter”), can be ...
oct8
... At the rate that the Sun is emitting energy, the Sun must have been much hotter just a few hundred years earlier, making life on Earth impossible. The Sun must have an energy source; a way of generating its own heat. ...
... At the rate that the Sun is emitting energy, the Sun must have been much hotter just a few hundred years earlier, making life on Earth impossible. The Sun must have an energy source; a way of generating its own heat. ...
Apparent size (apparent diameter)
... 2. The apparent path of the sun through the sky is an arc. 3. In the U.S. the sun, the moon, and all of the stars appear to rise from the ___________ horizon, move through the southern sky, and set in the ___________________. (think daily motion disco) 4. The noon sun is ________________ at the zeni ...
... 2. The apparent path of the sun through the sky is an arc. 3. In the U.S. the sun, the moon, and all of the stars appear to rise from the ___________ horizon, move through the southern sky, and set in the ___________________. (think daily motion disco) 4. The noon sun is ________________ at the zeni ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.