B - Department of Physics and Astronomy
... 16. Glitches are occasionally observed by astronomers studying pulsars. What are these glitches? A. clumps of denser material in the jets emitted along the magnetic poles B. sudden flares caused by matter falling onto the surface of the neutron star C. secondary pulses of radiation occasionally int ...
... 16. Glitches are occasionally observed by astronomers studying pulsars. What are these glitches? A. clumps of denser material in the jets emitted along the magnetic poles B. sudden flares caused by matter falling onto the surface of the neutron star C. secondary pulses of radiation occasionally int ...
Grzegorz F - (EU
... small, and the light did not have the nature of the wave and did not result in the phenomenon of diffraction at the edges of the diaphragm. - Real, because the image cast on the screen is made up by the actual light rays coming from the observed object. - Inverted, because the ray of the upper part ...
... small, and the light did not have the nature of the wave and did not result in the phenomenon of diffraction at the edges of the diaphragm. - Real, because the image cast on the screen is made up by the actual light rays coming from the observed object. - Inverted, because the ray of the upper part ...
Handy Pinhole Camera (Latin Camera Obscura) - (EU
... infinitely small, and the light did not have the nature of the wave and did not result in the phenomenon of diffraction at the edges of the diaphragm. - Real, because the image cast on the screen is made up by the actual light rays coming from the observed object. - Inverted, because the ray of the ...
... infinitely small, and the light did not have the nature of the wave and did not result in the phenomenon of diffraction at the edges of the diaphragm. - Real, because the image cast on the screen is made up by the actual light rays coming from the observed object. - Inverted, because the ray of the ...
Hertzsprung-Russell Diagram—key to understanding properties of stars. 26 Sept
... You are a young astronomer in 1890, and you want to study stars. The distances to a few dozen stars are known. How do you attack this problem? What characteristics of stars do you see in the pictures of the Orion constellation and a globular cluster (taken 100 years later)? ...
... You are a young astronomer in 1890, and you want to study stars. The distances to a few dozen stars are known. How do you attack this problem? What characteristics of stars do you see in the pictures of the Orion constellation and a globular cluster (taken 100 years later)? ...
虚拟天文台引领天文学网络化协同工作 - Chinese Virtual Observatory
... • SDSS DR5 photometric data were searched for new Milky Way companions or substructures in the Galactic halo. • Data analysis procedures were based on the VO-DAS. • Five candidates are identified as over-dense faint stellar sources that have color-magnitude diagrams similar to those of known globula ...
... • SDSS DR5 photometric data were searched for new Milky Way companions or substructures in the Galactic halo. • Data analysis procedures were based on the VO-DAS. • Five candidates are identified as over-dense faint stellar sources that have color-magnitude diagrams similar to those of known globula ...
Scientific American`s Ask the Experts
... craft to encounter an asteroid while it was passing through the asteroid belt on its way to Jupiter. But it took some effort to find an object that was located even roughly along Galileo’s path. Special targeting was required to reach this object, but the result was the first close-up view of an aster ...
... craft to encounter an asteroid while it was passing through the asteroid belt on its way to Jupiter. But it took some effort to find an object that was located even roughly along Galileo’s path. Special targeting was required to reach this object, but the result was the first close-up view of an aster ...
V - ESO
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
... This is generally assumed to be the reason why, though star formation proceeds on a typical scale comparable to the size of a giant molecular cloud (~80 pc, Efremov 1995, AJ 100, 2757), Milky Way massive clusters tend to be much smaller. Image taken from class by James Schombert, University of Oreg ...
Final review - Physics and Astronomy
... When we record a photon from a distant source, its wavelength will be longer. This is like the Doppler Shift, but it is not due to relative motion of source and receiver. This is correct way to think of redshifts of galaxies. ...
... When we record a photon from a distant source, its wavelength will be longer. This is like the Doppler Shift, but it is not due to relative motion of source and receiver. This is correct way to think of redshifts of galaxies. ...
Andromeda Check-List - Norman Lockyer Observatory
... A lovely object when viewed through moderate sized telescopes. The cluster consists of a number of bright rich stars in a wedge shaped formation. NGC188/ Collinder 6/Caldwell 1 – Open Cluster – II 2 r – Moderate Not visible to the naked eye but easily seen through binoculars it will appear as a fain ...
... A lovely object when viewed through moderate sized telescopes. The cluster consists of a number of bright rich stars in a wedge shaped formation. NGC188/ Collinder 6/Caldwell 1 – Open Cluster – II 2 r – Moderate Not visible to the naked eye but easily seen through binoculars it will appear as a fain ...
The Milky Way
... • You ARE responsible for understanding the topics covered in class (including details in the book that I may not have mentioned). • You are NOT responsible for other stuff in these chapters not covered at all in lecture. ...
... • You ARE responsible for understanding the topics covered in class (including details in the book that I may not have mentioned). • You are NOT responsible for other stuff in these chapters not covered at all in lecture. ...
Implications of the Search and Discovery of Life in the Universe
... Number of Intelligent Civilizations = Number of Stars in the Galaxy (400 billion) x Fraction of Stars with Planets (1/4?) x Number of suitable planets per star (2?) x Fraction of planets where life appears (1/2??) x Fraction of planets with intelligence (???) x Fraction of planets with technology (? ...
... Number of Intelligent Civilizations = Number of Stars in the Galaxy (400 billion) x Fraction of Stars with Planets (1/4?) x Number of suitable planets per star (2?) x Fraction of planets where life appears (1/2??) x Fraction of planets with intelligence (???) x Fraction of planets with technology (? ...
The Sky Above: A First Look
... The program begins by showing several students looking through a telescope at the night sky. The program defines the sky as everything above Earth's surface. It introduces the things most obvious to the students: the stars, planets, sun, and moon. The video explains that many of the stars we see are ...
... The program begins by showing several students looking through a telescope at the night sky. The program defines the sky as everything above Earth's surface. It introduces the things most obvious to the students: the stars, planets, sun, and moon. The video explains that many of the stars we see are ...
Implications of the Search and Discovery
... Number of Intelligent Civilizations = Number of Stars in the Galaxy (400 billion) x Fraction of Stars with Planets (1/4?) x Number of suitable planets per star (2?) x Fraction of planets where life appears (1/2??) x Fraction of planets with intelligence (???) x Fraction of planets with technology (? ...
... Number of Intelligent Civilizations = Number of Stars in the Galaxy (400 billion) x Fraction of Stars with Planets (1/4?) x Number of suitable planets per star (2?) x Fraction of planets where life appears (1/2??) x Fraction of planets with intelligence (???) x Fraction of planets with technology (? ...
Teacher Guide Lives of Stars
... which these stars differ as they progress through their various stages of life and death. A star, like our Sun, is an enormous and complex system. In order to model and understand their properties and how they change with time, astronomers and astrophysicists apply the basic ideas in physics to math ...
... which these stars differ as they progress through their various stages of life and death. A star, like our Sun, is an enormous and complex system. In order to model and understand their properties and how they change with time, astronomers and astrophysicists apply the basic ideas in physics to math ...
Origin of the Elements
... (Ne), magnesium (Mg), oxygen (O), sulfur (S), and silicon (Si) are formed in the outer layers. The heavier elements are formed closer to the core and eventually fuse in the core of the star to form iron (Fe), the most massive element found in stars. ...
... (Ne), magnesium (Mg), oxygen (O), sulfur (S), and silicon (Si) are formed in the outer layers. The heavier elements are formed closer to the core and eventually fuse in the core of the star to form iron (Fe), the most massive element found in stars. ...
PRS Questions (queestions after Midterm 2)
... half-life of 10 years. If 30 years later you stumble across that stuff, you will find that you still have ...
... half-life of 10 years. If 30 years later you stumble across that stuff, you will find that you still have ...
NASA Launches Space Shuttle on Historic Final Mission House
... shown here. Get your telescope on all these objects early; they move lower later in the evening. Saturday, July 9 · Titan, the brightest satellite of Saturn, can be found in a telescope about four ring-lengths west of Saturn this evening and tomorrow evening. With an aperture of 6 inches or more, yo ...
... shown here. Get your telescope on all these objects early; they move lower later in the evening. Saturday, July 9 · Titan, the brightest satellite of Saturn, can be found in a telescope about four ring-lengths west of Saturn this evening and tomorrow evening. With an aperture of 6 inches or more, yo ...
Mark Scheme (Results) Summer 2016 - Edexcel
... Very accurate measurement of star’s position / astrometry To detect tiny ‘wiggles’ as it is orbited by planet or Radial velocity / Doppler measurement To detect tiny ‘wiggles’ as it is orbited by planet ...
... Very accurate measurement of star’s position / astrometry To detect tiny ‘wiggles’ as it is orbited by planet or Radial velocity / Doppler measurement To detect tiny ‘wiggles’ as it is orbited by planet ...
Lecture Ten - The Sun Amongst the Stars Part II
... O-type stars have very few lines because they are so hot that most of their elements have been stripped of electrons – while in cooler, M-type stars, far more atoms retain their electrons. Patterns of absorption lines can reveal the temperatures of the stars to a precision within 50 degrees K – a f ...
... O-type stars have very few lines because they are so hot that most of their elements have been stripped of electrons – while in cooler, M-type stars, far more atoms retain their electrons. Patterns of absorption lines can reveal the temperatures of the stars to a precision within 50 degrees K – a f ...
Active Galactic Nuclei
... Quasars are observed only at high redshifts – at large lookback times, so they existed in the distant past. There are no nearby quasars. The lower luminosity AGN’s, the Seyfert and starburst galaxies, bridge the gap between us and the more distant quasars ...
... Quasars are observed only at high redshifts – at large lookback times, so they existed in the distant past. There are no nearby quasars. The lower luminosity AGN’s, the Seyfert and starburst galaxies, bridge the gap between us and the more distant quasars ...
International Ultraviolet Explorer
The International Ultraviolet Explorer (IUE) was an astronomical observatory satellite primarily designed to take ultraviolet spectra. The satellite was a collaborative project between NASA, the UK Science Research Council and the European Space Agency (ESA). The mission was first proposed in early 1964, by a group of scientists in the United Kingdom, and was launched on January 26, 1978 aboard a NASA Delta rocket. The mission lifetime was initially set for 3 years, but in the end it lasted almost 18 years, with the satellite being shut down in 1996. The switch-off occurred for financial reasons, while the telescope was still functioning at near original efficiency.It was the first space observatory to be operated in real time by astronomers who visited the groundstations in the United States and Europe. Astronomers made over 104,000 observations using the IUE, of objects ranging from solar system bodies to distant quasars. Among the significant scientific results from IUE data were the first large scale studies of stellar winds, accurate measurements of the way interstellar dust absorbs light, and measurements of the supernova SN1987A which showed that it defied stellar evolution theories as they then stood. When the mission ended, it was considered the most successful astronomical satellite ever.