Astronomy (stars, galaxies and the Universe)
... White dwarfs- smaller than the Earth (ex. Van Maanen’s star) Medium-sized stars- vary in size from 1/10 to 10 times the size of the Sun (ex. the Sun & Sirius) Giant stars- 10 to 100 times as large as the Sun (ex. Aldebara) Supergiant stars- up to 1000 times larger than the Sun (ex. Rigel & Betelgeus ...
... White dwarfs- smaller than the Earth (ex. Van Maanen’s star) Medium-sized stars- vary in size from 1/10 to 10 times the size of the Sun (ex. the Sun & Sirius) Giant stars- 10 to 100 times as large as the Sun (ex. Aldebara) Supergiant stars- up to 1000 times larger than the Sun (ex. Rigel & Betelgeus ...
The universe is faster, colder, and wackier than anything we can
... that any object in the universe exerts, and yet is still able to force another body to orbit it? Many small galaxies have correspondingly weak gravity. But if two low-mass galaxies can somehow come together in an isolated region of space such that they can move without being affected by larger galaxi ...
... that any object in the universe exerts, and yet is still able to force another body to orbit it? Many small galaxies have correspondingly weak gravity. But if two low-mass galaxies can somehow come together in an isolated region of space such that they can move without being affected by larger galaxi ...
Stars - WhatisOutThere
... Is the sun a star? How? The sun is like any other star, it has an average size and temperature, and shines as bright as other stars do. Some stars are bigger and hotter and some a smaller and cooler. Like our sun there are billions of stars in our universe. We need the sun because it is our source ...
... Is the sun a star? How? The sun is like any other star, it has an average size and temperature, and shines as bright as other stars do. Some stars are bigger and hotter and some a smaller and cooler. Like our sun there are billions of stars in our universe. We need the sun because it is our source ...
Goal: To understand how we know distances to
... brightness (the rotation gives an indication of mass which therefore would affect brightness). • The rotation is found using the Doppler shifts of the 21 cm line of Hydrogen. • You can also use bright objects such as very massive stars, novae, and some supernova. • There is also some who think the s ...
... brightness (the rotation gives an indication of mass which therefore would affect brightness). • The rotation is found using the Doppler shifts of the 21 cm line of Hydrogen. • You can also use bright objects such as very massive stars, novae, and some supernova. • There is also some who think the s ...
Goal: To understand how we know distances to various
... brightness (the rotation gives an indication of mass which therefore would affect brightness). • The rotation is found using the Doppler shifts of the 21 cm line of Hydrogen. • You can also use bright objects such as very massive stars, novae, and some supernova. • There is also some who think the s ...
... brightness (the rotation gives an indication of mass which therefore would affect brightness). • The rotation is found using the Doppler shifts of the 21 cm line of Hydrogen. • You can also use bright objects such as very massive stars, novae, and some supernova. • There is also some who think the s ...
γ The potential for intensity interferometry with -ray telescope arrays
... mv ≈ 8.5m for a S/N = 5, and a 5 hours integration in case of 50% visibility (see Le Bohec et al., these proceedings). These specifications allow important interferometric studies regarding binary stars, stellar radii and pulsating stars with unprecedented resolution on scales of 10s of µ -arcsecond ...
... mv ≈ 8.5m for a S/N = 5, and a 5 hours integration in case of 50% visibility (see Le Bohec et al., these proceedings). These specifications allow important interferometric studies regarding binary stars, stellar radii and pulsating stars with unprecedented resolution on scales of 10s of µ -arcsecond ...
Chapter 29 Notes-
... • Dark lines form in the spectra of stars when gases in the stars’ outer layers absorb specific wavelengths of the light that passes through the layers. • By studying the spectrum of a star, scientists can determine the amounts of elements that are present in a star’s atmosphere • Because each eleme ...
... • Dark lines form in the spectra of stars when gases in the stars’ outer layers absorb specific wavelengths of the light that passes through the layers. • By studying the spectrum of a star, scientists can determine the amounts of elements that are present in a star’s atmosphere • Because each eleme ...
Ch. S1 - Relativity Group
... First of all, the beauty that he sees is available to other people and to me, too, I believe, although I might not be quite as refined aesthetically as he is. But I can appreciate the beauty of a flower. At the same time, I see much more about the flower that he sees. I could imagine the cells in th ...
... First of all, the beauty that he sees is available to other people and to me, too, I believe, although I might not be quite as refined aesthetically as he is. But I can appreciate the beauty of a flower. At the same time, I see much more about the flower that he sees. I could imagine the cells in th ...
W > 1 - The Open University
... telescope used. If you find the Moon too bright use a filter to reduce the glare. At times features along different parts of the limb are better presented due the effect of libration – an apparent wobbling of the Moon about its axis – that allows us to see about 59% of its surface. The BAA Handbook ...
... telescope used. If you find the Moon too bright use a filter to reduce the glare. At times features along different parts of the limb are better presented due the effect of libration – an apparent wobbling of the Moon about its axis – that allows us to see about 59% of its surface. The BAA Handbook ...
Slide 1
... massive objects settle onto the main sequence, where they burned hydrogen into helium. After burning helium into carbon, stars run out of fuel and collapse into white dwarf stars, producing beautiful planetary nebulae in the process. ...
... massive objects settle onto the main sequence, where they burned hydrogen into helium. After burning helium into carbon, stars run out of fuel and collapse into white dwarf stars, producing beautiful planetary nebulae in the process. ...
Powerpoint Presentation (large file)
... increase in luminosity that we call a nova • The peak luminosity of a nova is only 10–4 of that observed in a supernova • Explosive helium fusion may occur in the surface layer of a companion neutron star • This produces a sudden increase in X-ray radiation, which we call a burster ...
... increase in luminosity that we call a nova • The peak luminosity of a nova is only 10–4 of that observed in a supernova • Explosive helium fusion may occur in the surface layer of a companion neutron star • This produces a sudden increase in X-ray radiation, which we call a burster ...
presentation source
... “This, I imagine, is why the oldest members of the stellar system…are so large and populous, for the available material was richer then. As the layer of dust and gas sank toward the galactic plane, stars continued to form. Dust and gas still lie dense in this layer, and stars are still being formed ...
... “This, I imagine, is why the oldest members of the stellar system…are so large and populous, for the available material was richer then. As the layer of dust and gas sank toward the galactic plane, stars continued to form. Dust and gas still lie dense in this layer, and stars are still being formed ...
Lecture 1 Coordinate Systems - Department of Physics & Astronomy
... •Not measured until 1838 by Friedrich Wilhelm Bessel •Hipparcos satellite measurement accuracy approaches 0.001” for over 118,000 stars. This corresponds to a a distance of only 1000 pc (only 1/8 of way to centerof our galaxy) •The planned Space Interferometry Mission will be able to determine paral ...
... •Not measured until 1838 by Friedrich Wilhelm Bessel •Hipparcos satellite measurement accuracy approaches 0.001” for over 118,000 stars. This corresponds to a a distance of only 1000 pc (only 1/8 of way to centerof our galaxy) •The planned Space Interferometry Mission will be able to determine paral ...
Spectroscope Lab
... The wavelength of light that an observer sees coming from an object depends on the motion of the object relative to the observer. If either the object or the observer moves, the wavelength will change. The relationship between motion and observed wavelength is called the Doppler effect. ...
... The wavelength of light that an observer sees coming from an object depends on the motion of the object relative to the observer. If either the object or the observer moves, the wavelength will change. The relationship between motion and observed wavelength is called the Doppler effect. ...
Solar-like oscillations in intermediate red giants
... There are modes with inertia similar to that of a radial modes. In principle, this modes might be excited to an observable level throught stochastic ...
... There are modes with inertia similar to that of a radial modes. In principle, this modes might be excited to an observable level throught stochastic ...
How We Know the Earth Revolves Activity
... How do scientists know that the Earth actually orbits (revolves about) the sun? Have you ever thought about this? For thousands of years it was thought that the Earth was at the center of the universe and that everything moved around the Earth at different rates. Today, scientists know that the Eart ...
... How do scientists know that the Earth actually orbits (revolves about) the sun? Have you ever thought about this? For thousands of years it was thought that the Earth was at the center of the universe and that everything moved around the Earth at different rates. Today, scientists know that the Eart ...
HR Diagram Explorer
... 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 control the variables plotted on the x-axis: (temperature, B-V, or spectral type) and those plotted on the y-ax ...
... 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 control the variables plotted on the x-axis: (temperature, B-V, or spectral type) and those plotted on the y-ax ...
1” “Sky-Notes” of the Open University Astronomy Club. June 2005. A
... the Moon too bright use a filter to reduce the glare. At times features along different parts of the limb are better presented due the effect of libration – an apparent wobbling of the Moon about its axis – that allows us to see about 59% of its surface. The BAA Handbook and some monthly magazines ( ...
... the Moon too bright use a filter to reduce the glare. At times features along different parts of the limb are better presented due the effect of libration – an apparent wobbling of the Moon about its axis – that allows us to see about 59% of its surface. The BAA Handbook and some monthly magazines ( ...
Galaxy Far Far Away ppt
... HALO: Area surrounding galaxy that contains some scattered globular clusters. DISK: Contains most of the stars in the galaxy. ...
... HALO: Area surrounding galaxy that contains some scattered globular clusters. DISK: Contains most of the stars in the galaxy. ...
W > 1 - The Open University
... Test your eyesight from a dark site by counting the number of naked eye stars that are visible. Seven should readily be seen. Keen vision will lead you into double figures. A test for moderate apertures is the nebulosity around some of the other brighter stars of the group, especially Merope. Nebula ...
... Test your eyesight from a dark site by counting the number of naked eye stars that are visible. Seven should readily be seen. Keen vision will lead you into double figures. A test for moderate apertures is the nebulosity around some of the other brighter stars of the group, especially Merope. Nebula ...
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.