ASTR3007/4007/6007: Part I: Stars Semester 1, 2017 Problem set 1
... (e) [4 points] Assume that the material in the star is a monatomic ideal gas. Calculate the total internal energy of the star from P (r), and show that the virial theorem is satisfied. 4. Powering Jupiter by Gravity. [10 points] The Sun is in thermal equilibrium because its thermal timescale is shor ...
... (e) [4 points] Assume that the material in the star is a monatomic ideal gas. Calculate the total internal energy of the star from P (r), and show that the virial theorem is satisfied. 4. Powering Jupiter by Gravity. [10 points] The Sun is in thermal equilibrium because its thermal timescale is shor ...
Lecture12
... Convection A bubble of gas that is lower density than its surroundings will rise buoyantly From the ideal gas law: if gas is in approximate pressure equilibrium (i.e. not expanding or contracting) then pockets of gas that are hotter than their surroundings will also be less dense. ...
... Convection A bubble of gas that is lower density than its surroundings will rise buoyantly From the ideal gas law: if gas is in approximate pressure equilibrium (i.e. not expanding or contracting) then pockets of gas that are hotter than their surroundings will also be less dense. ...
High Resolution Observations of Hot Molecular Cores
... Very common Keplerian Selfgravitating ...
... Very common Keplerian Selfgravitating ...
doc - EU-HOU
... 6. Copy and rename the Excel file Answerfile_radialvel_empty.xls. 7. You can notice two deep absorption lines of sodium (Na) close to 589.0 nm and 589.6 nm. There is a smaller one (from nickel) at 589.3 nm (we shall not use this one). Measure the position of the two Na lines more precisely. The bes ...
... 6. Copy and rename the Excel file Answerfile_radialvel_empty.xls. 7. You can notice two deep absorption lines of sodium (Na) close to 589.0 nm and 589.6 nm. There is a smaller one (from nickel) at 589.3 nm (we shall not use this one). Measure the position of the two Na lines more precisely. The bes ...
Slide 1
... Explanation: Microquasars, bizarre binary star systems generating high-energy radiation and blasting out jets of particles at nearly the speed of light, live in our Milky Way galaxy. The energetic microquasar systems seem to consist of a very compact object, either a neutron star or a black hole, f ...
... Explanation: Microquasars, bizarre binary star systems generating high-energy radiation and blasting out jets of particles at nearly the speed of light, live in our Milky Way galaxy. The energetic microquasar systems seem to consist of a very compact object, either a neutron star or a black hole, f ...
Lecture 38. The Fermi Paradox, Von Neumann Machines
... "it contained speculations which were too remote from reality". Thus, Fermi saw the theory published in Italian and in German before it was published in English. He never forgot this experience of being ahead of his time, and used to tell his protégés: "Never be first; try to be second".’ ...
... "it contained speculations which were too remote from reality". Thus, Fermi saw the theory published in Italian and in German before it was published in English. He never forgot this experience of being ahead of his time, and used to tell his protégés: "Never be first; try to be second".’ ...
ESO telescopes
... Including the central star, disk, and envelope, these models can provide a much more comprehensive and consistent picture of the IRAS 13481-6124 system. Given that these models depend on many free parameters, we employed a pre-computed grid of radiative transfer simulations23 and an associated SED-f ...
... Including the central star, disk, and envelope, these models can provide a much more comprehensive and consistent picture of the IRAS 13481-6124 system. Given that these models depend on many free parameters, we employed a pre-computed grid of radiative transfer simulations23 and an associated SED-f ...
Astrophysics - Mr Priest`s Physics Notes
... Infrared astronomers study parts of the infrared spectrum, which consists of electromagnetic waves with wavelengths ranging from just longer than visible light to 1,000 times longer than visible light. Earth’s atmosphere absorbs infrared radiation, so astronomers must collect infrared radiation from ...
... Infrared astronomers study parts of the infrared spectrum, which consists of electromagnetic waves with wavelengths ranging from just longer than visible light to 1,000 times longer than visible light. Earth’s atmosphere absorbs infrared radiation, so astronomers must collect infrared radiation from ...
Spectroscopy
... useful in helping understand how an object like a Star or active galaxy is producing light, how fast it is moving, and even what elements it is made of • A spectrum is simply a chart or a graph that shows the intensity of light being emitted over a range of energies • Spectra can be produced for any ...
... useful in helping understand how an object like a Star or active galaxy is producing light, how fast it is moving, and even what elements it is made of • A spectrum is simply a chart or a graph that shows the intensity of light being emitted over a range of energies • Spectra can be produced for any ...
Physics 161 Homework 8 - Solutions Wednesday
... P/ρ, inside a white dwarf. In an accreting white dwarf vS = with a carbon core that has reached nuclear ignition temperatyure, a nuclear binding “flame” emcompases the star at the sound velocity or faster. Within how much time, in seconds, does the flame traverse the radius of the white dwarf, assum ...
... P/ρ, inside a white dwarf. In an accreting white dwarf vS = with a carbon core that has reached nuclear ignition temperatyure, a nuclear binding “flame” emcompases the star at the sound velocity or faster. Within how much time, in seconds, does the flame traverse the radius of the white dwarf, assum ...
At the Heart of the Matter: The Blue White Dwarf in M 57. Paul Temple
... elements may be observed in smaller amounts. DB This class may be regarded as an extension of the DO group into lower temperature regions (below around 30,000K). The cooler temperatures are insufficient to ionise helium, and so the spectrum is dominated by He I, with only trace amounts of H (only 1/ ...
... elements may be observed in smaller amounts. DB This class may be regarded as an extension of the DO group into lower temperature regions (below around 30,000K). The cooler temperatures are insufficient to ionise helium, and so the spectrum is dominated by He I, with only trace amounts of H (only 1/ ...
Neutron Stars and Black Holes
... • Mass of billions of stars in size of SS (Kepler’s 3rd Law). • Black hole likely in center of the Milky Way. ...
... • Mass of billions of stars in size of SS (Kepler’s 3rd Law). • Black hole likely in center of the Milky Way. ...
Astronomy 112: The Physics of Stars Class 19 Notes: The Stellar
... older stellar population. Given a bunch of stars in an HR diagram this technique can get quite sophisticated. An example is a recent paper by Williams et al. that used this method to determine the star formation history in different parts of a nearby galaxy. They divided the galaxy into annuli, and ...
... older stellar population. Given a bunch of stars in an HR diagram this technique can get quite sophisticated. An example is a recent paper by Williams et al. that used this method to determine the star formation history in different parts of a nearby galaxy. They divided the galaxy into annuli, and ...
Characteristics of Stars - Laconia School District
... • How do astronomers measure distance to the stars? • Astronomers use a method called parallax. Because of the Earth's revolution about the sun, near stars seem to shift their position against the farther stars. The smaller the parallax shift, the farther away from earth the star is. This method is ...
... • How do astronomers measure distance to the stars? • Astronomers use a method called parallax. Because of the Earth's revolution about the sun, near stars seem to shift their position against the farther stars. The smaller the parallax shift, the farther away from earth the star is. This method is ...
Powerpoint file
... of intelligence and technology and try to communicate), we are calculating the number of life-bearing planets in our Galaxy at any given time (like now). We know there has been life on our planet for 3 billion years, so take L = 3 billion. Let’s be optimistic about fP (0.1), nP (1), and fL= (0.1). T ...
... of intelligence and technology and try to communicate), we are calculating the number of life-bearing planets in our Galaxy at any given time (like now). We know there has been life on our planet for 3 billion years, so take L = 3 billion. Let’s be optimistic about fP (0.1), nP (1), and fL= (0.1). T ...
Stages 7 to 9 - Sun
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
Astronomy Syllabus - Jefferson Forest High School
... Estimation of Stellar sizes H-R Diagram Composition and physical properties of the interstellar medium Characteristics of emission nebulae Properties of dark interstellar clouds Theory of star formation Effect of mass on star formation Evolutionary stages followed by a Sun-like star Evolutionary sta ...
... Estimation of Stellar sizes H-R Diagram Composition and physical properties of the interstellar medium Characteristics of emission nebulae Properties of dark interstellar clouds Theory of star formation Effect of mass on star formation Evolutionary stages followed by a Sun-like star Evolutionary sta ...
H-R Diagram
... To identify the characteristics of a star from data in the diagram To classify a star by its position in the diagram To compare the life cycle stages of stars based on their positions in the diagram Background The Hertzsprung-Russell diagram, or H-R diagram, is a graph in which a star's temperature ...
... To identify the characteristics of a star from data in the diagram To classify a star by its position in the diagram To compare the life cycle stages of stars based on their positions in the diagram Background The Hertzsprung-Russell diagram, or H-R diagram, is a graph in which a star's temperature ...
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.