Ch_16-18_Example_Exam
... ____ 29. What is the meaning of the Schwarzschild radius around a black hole? a. It is the radius at which an orbiting object would show a precession. b. It is the radius at which gravitational redshift can be detected. c. It is the radius at which the black hole’s spin equals the speed of light. d. ...
... ____ 29. What is the meaning of the Schwarzschild radius around a black hole? a. It is the radius at which an orbiting object would show a precession. b. It is the radius at which gravitational redshift can be detected. c. It is the radius at which the black hole’s spin equals the speed of light. d. ...
Diffraction-of-light
... The amount of bending depends on the relative size of the wavelength of light to the size of the opening. If the opening is much larger than the light’s wavelength, the bending will be almost unnoticeable. However, if the two are closer in size or equal, the amount of bending is considerable, and ea ...
... The amount of bending depends on the relative size of the wavelength of light to the size of the opening. If the opening is much larger than the light’s wavelength, the bending will be almost unnoticeable. However, if the two are closer in size or equal, the amount of bending is considerable, and ea ...
Stellar Spectroscopy during Exoplanet Transits
... Line profile changes during exoplanet transit. Red: Ratios of line profiles relative to the profile outside transit. This simulation sequence from a CO5BOLD model predicts the behavior of an Fe I line ( 620 nm, = 3 eV) during the first half of a transit across the stellar equator by a bloated Jup ...
... Line profile changes during exoplanet transit. Red: Ratios of line profiles relative to the profile outside transit. This simulation sequence from a CO5BOLD model predicts the behavior of an Fe I line ( 620 nm, = 3 eV) during the first half of a transit across the stellar equator by a bloated Jup ...
ISOCAM 4 m imaging of the nuclear starburst in M83
... The observations, performed with the short wavelength channel of ISOCAM (Cesarsky et al., 1996), the camera onboard ISO (Kesslet et al., 1996) , took place at the very end of the Preliminary Verification (PV) phase of ISO in January 1996. The pixel field of view was 1.5 arcsec and the observations d ...
... The observations, performed with the short wavelength channel of ISOCAM (Cesarsky et al., 1996), the camera onboard ISO (Kesslet et al., 1996) , took place at the very end of the Preliminary Verification (PV) phase of ISO in January 1996. The pixel field of view was 1.5 arcsec and the observations d ...
Engineering the Heavens
... theory of instrumental errors, which effectively created the full range of possible observing conditions. Why? As a new art of observation. Defects that can be measured wonderfully summarized by one nineteenth-century writer and allowed for are as good as nonexistent. In December in The North Americ ...
... theory of instrumental errors, which effectively created the full range of possible observing conditions. Why? As a new art of observation. Defects that can be measured wonderfully summarized by one nineteenth-century writer and allowed for are as good as nonexistent. In December in The North Americ ...
Types of Stars http://space.about.com/od/stars/tp/What-Are
... Astronomers estimate that some red dwarf stars will burn for up to 10 trillion years. The smallest red dwarfs are 0.075 times the mass of the Sun, and they can have a mass of up to half of the Sun. 11. Supergiant Stars The largest stars in the Universe are supergiant stars. These are monsters with ...
... Astronomers estimate that some red dwarf stars will burn for up to 10 trillion years. The smallest red dwarfs are 0.075 times the mass of the Sun, and they can have a mass of up to half of the Sun. 11. Supergiant Stars The largest stars in the Universe are supergiant stars. These are monsters with ...
The K Integral and Radiation Pressure
... Specific intensity/mean intensity Flux The K integral and radiation pressure Absorption coefficient/optical depth Emission coefficient The source function The transfer equation & examples Einstein coefficients ...
... Specific intensity/mean intensity Flux The K integral and radiation pressure Absorption coefficient/optical depth Emission coefficient The source function The transfer equation & examples Einstein coefficients ...
WBL6_Lecture_Ch27
... Planck realized that the ultraviolet catastrophe goes away if we assume that the possible values of the energy of electromagnetic radiation are not continuous, but rather come in little “packets,” whose energies are given by: ...
... Planck realized that the ultraviolet catastrophe goes away if we assume that the possible values of the energy of electromagnetic radiation are not continuous, but rather come in little “packets,” whose energies are given by: ...
Problem Set No. 5
... 2. Why do some astronomers say that brown dwarfs are not really stars? Why are brown dwarfs hard to study? Some astronomers would say that true stars must have nuclear fusion as an internal energy source. Brown dwarfs are too cool the burn hydrogen. Even though there are nearby brown dwarfs, their ...
... 2. Why do some astronomers say that brown dwarfs are not really stars? Why are brown dwarfs hard to study? Some astronomers would say that true stars must have nuclear fusion as an internal energy source. Brown dwarfs are too cool the burn hydrogen. Even though there are nearby brown dwarfs, their ...
doc
... [The lucky placement of a “resonance” without which there would be no carbon or anything heavier is discussed in class.] This reaction requires T~100 million degrees K, which the core has attained by its contraction and heating. But for low mass stars (less than about 2 Mo), when the He gets hot eno ...
... [The lucky placement of a “resonance” without which there would be no carbon or anything heavier is discussed in class.] This reaction requires T~100 million degrees K, which the core has attained by its contraction and heating. But for low mass stars (less than about 2 Mo), when the He gets hot eno ...
What is a star?
... • Stars have different sizes, ranging from 1/100 the size of the sun to 1,000 times the size of the sun. • Two or more stars may be bound together by gravity, which causes them to orbit each other. • Three or more stars that are bound by gravity are called multiple stars or multiple star systems. T ...
... • Stars have different sizes, ranging from 1/100 the size of the sun to 1,000 times the size of the sun. • Two or more stars may be bound together by gravity, which causes them to orbit each other. • Three or more stars that are bound by gravity are called multiple stars or multiple star systems. T ...
File - Physical Science
... Stars make up 99% of the total VISIBLE matter in the Universe. Therefore, 99% of everything VISIBLE that exists in the entire Universe is in the plasma state. ...
... Stars make up 99% of the total VISIBLE matter in the Universe. Therefore, 99% of everything VISIBLE that exists in the entire Universe is in the plasma state. ...
ALUMINIUM-26 IN THE EARLY SOLAR SYSTEM : A PROBABILITY
... when massive stars are ready to explode as SNe, they are surrounded by HII regions of radius a few pc where star formation does not occur [21]. If that constraint had been taken into account by [7, 8], the probability estimate for a single SN would have been close to zero. The number of a few % is i ...
... when massive stars are ready to explode as SNe, they are surrounded by HII regions of radius a few pc where star formation does not occur [21]. If that constraint had been taken into account by [7, 8], the probability estimate for a single SN would have been close to zero. The number of a few % is i ...
PPTX
... Fabry-Pérots (tunable filters) Fabry-Pérot imaging spectrographs are different from what is usually meant by integral field spectroscopy, but the result is still a data-cube. Fabry-Pérots allow a large FoV (e.g. 5 arcmin) to be surveyed at high spatial resolution (e.g. 0.3 arcmin/pixel) in a si ...
... Fabry-Pérots (tunable filters) Fabry-Pérot imaging spectrographs are different from what is usually meant by integral field spectroscopy, but the result is still a data-cube. Fabry-Pérots allow a large FoV (e.g. 5 arcmin) to be surveyed at high spatial resolution (e.g. 0.3 arcmin/pixel) in a si ...
Science Olympiad 2011 Practice Optics C
... 15. Which color of visible light bends the most in a prism? 16. In the year 1800, William Herschel set up a prism to separate light from the sun into its different colors. He set up several thermometers in the way of the dispersed beam, as well as one just beyond red, where there was no color. To hi ...
... 15. Which color of visible light bends the most in a prism? 16. In the year 1800, William Herschel set up a prism to separate light from the sun into its different colors. He set up several thermometers in the way of the dispersed beam, as well as one just beyond red, where there was no color. To hi ...
PHYSICS 113 Practice Questions #2
... c. HII regions -- clouds of ionized hydrogen d. interstellar grains e. all these clouds are approximately the same size 11. Astronomers use the term interstellar extinction to refer to: a. the death o f the dinosaur s and other species from the collision of a n asteroid w ith the Earth b. the death ...
... c. HII regions -- clouds of ionized hydrogen d. interstellar grains e. all these clouds are approximately the same size 11. Astronomers use the term interstellar extinction to refer to: a. the death o f the dinosaur s and other species from the collision of a n asteroid w ith the Earth b. the death ...
gravPart2
... Lec12: Growth of a Black Hole by capturing objects in Loss Cone • A small BH on orbit with pericentre rp
... Lec12: Growth of a Black Hole by capturing objects in Loss Cone • A small BH on orbit with pericentre rp
Spiralicity and Motion on Cosmic Scale
... General relativity has recently been confirmed on the nearby universe [4]. The predicted gravitational redshift of relativity has been found from the astronomical findings on galactic clusters, where groups of thousands galaxies are held together by their own gravity field to bend the light and to c ...
... General relativity has recently been confirmed on the nearby universe [4]. The predicted gravitational redshift of relativity has been found from the astronomical findings on galactic clusters, where groups of thousands galaxies are held together by their own gravity field to bend the light and to c ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.