Quiz on Chapter 11
... 11-13. White dwarfs usually have surface temperatures well above 10,000 K, yet they have extremely low luminosity. Why is this? a) They are very far away. b) They have a very large surface area. c) They emit most of their radiation in the far infrared. d) They have a very small surface area. X 11-14 ...
... 11-13. White dwarfs usually have surface temperatures well above 10,000 K, yet they have extremely low luminosity. Why is this? a) They are very far away. b) They have a very large surface area. c) They emit most of their radiation in the far infrared. d) They have a very small surface area. X 11-14 ...
Project 4: The HR diagram. Open clusters
... of a star. From the figure, one sees that most stars fall along a diagonal strip from high temperature, high luminosity stars to low temperature, low luminosity stars. These are the main sequence stars. Our Sun is one of them. There are a few stars that are not in this diagonal strip. ...
... of a star. From the figure, one sees that most stars fall along a diagonal strip from high temperature, high luminosity stars to low temperature, low luminosity stars. These are the main sequence stars. Our Sun is one of them. There are a few stars that are not in this diagonal strip. ...
Rainbows and Atoms
... a) Radio, microwave, infrared, visible, UV, Xray, γray b) γray, Xray, UV, visible, infrared, microwave, radio c) Radio, infrared, visible, Xray, UV d) γray, infrared, microwave, radio, UV, visible, Xray e) Xray, UV, radio, microwave ...
... a) Radio, microwave, infrared, visible, UV, Xray, γray b) γray, Xray, UV, visible, infrared, microwave, radio c) Radio, infrared, visible, Xray, UV d) γray, infrared, microwave, radio, UV, visible, Xray e) Xray, UV, radio, microwave ...
Transcript - Chandra X
... Slide 7: More detailed information about the H-R diagram will be presented further along. Since the presentation of the deep sky objects includes their spectral class and luminosity classes, the H-R diagram terminology is given here for those unfamiliar with H-R diagrams. The H-R diagram is a plot ...
... Slide 7: More detailed information about the H-R diagram will be presented further along. Since the presentation of the deep sky objects includes their spectral class and luminosity classes, the H-R diagram terminology is given here for those unfamiliar with H-R diagrams. The H-R diagram is a plot ...
Why Study Cosmic Near Infrared Background? (1-4um)
... They claim that the excess near infrared background cannot originate from high-z galaxies, because such galaxies are not seen in high-z galaxy surveys. ...
... They claim that the excess near infrared background cannot originate from high-z galaxies, because such galaxies are not seen in high-z galaxy surveys. ...
Lecture 10 Spectra of Stars and Binaries
... Colors of Stars • Stars are made of hot, dense gas – Con$nuous spectrum from the lowest visible ...
... Colors of Stars • Stars are made of hot, dense gas – Con$nuous spectrum from the lowest visible ...
Stellar Relaxation Times
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
... center of the Galaxy is not gravitationally affected by other stars. On the other hand, giant molecular clouds have masses that are ~ 108 M. Although the number density of clouds is lower, it’s not 1016 times lower! The masses of these clouds are therefore high enough to scatter stars out of their ...
B – V
... A(li) = amount of interstellar absorption in magnitudes. Then the observed magnitudes mi and mj at two different wavelengths li and lj are related to the intrinsic magnitudes, mi0 and mj0 by the expressions: ...
... A(li) = amount of interstellar absorption in magnitudes. Then the observed magnitudes mi and mj at two different wavelengths li and lj are related to the intrinsic magnitudes, mi0 and mj0 by the expressions: ...
Open Houses at the Campus Observatory Astronomical Horizons Lecture
... It does not have enough mass to burn neon. The sun becomes degenerate The sun loses too much mass as a planetary nebula It takes too long to burn neon. ...
... It does not have enough mass to burn neon. The sun becomes degenerate The sun loses too much mass as a planetary nebula It takes too long to burn neon. ...
Numerical Star-Formation Studies-
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
ppt
... in the spin distribution of the LMXBs more than thirty years ago (Papaloizou & Pringle 1978). The main emission mechanisms that could be at work in these systems are crustal “mountains” (Bildsten 1998; Ushomirsky, Cutler & Bildsten 2000), magnetic deformations (Cutler 2002; Melatos & Payne 2005) or ...
... in the spin distribution of the LMXBs more than thirty years ago (Papaloizou & Pringle 1978). The main emission mechanisms that could be at work in these systems are crustal “mountains” (Bildsten 1998; Ushomirsky, Cutler & Bildsten 2000), magnetic deformations (Cutler 2002; Melatos & Payne 2005) or ...
Observations of V838 Mon light echo
... In classical novae, hydrogen explosion happens in a layer on a white dwarf surface. A small amount of matter located above being ejected into space has a mass of 1/1000 or 1/10000 solar masses. When the ejected gas expands, its density decreases rapidly, it passes into the optically thin state and g ...
... In classical novae, hydrogen explosion happens in a layer on a white dwarf surface. A small amount of matter located above being ejected into space has a mass of 1/1000 or 1/10000 solar masses. When the ejected gas expands, its density decreases rapidly, it passes into the optically thin state and g ...
Origin of Chemical Elements
... • What can we learn from telescopes? Modern telescopes (especially space telescopes) allow us to observe all the EM waves emitted by stars, not just visible ...
... • What can we learn from telescopes? Modern telescopes (especially space telescopes) allow us to observe all the EM waves emitted by stars, not just visible ...
Microsoft Word 97
... 3) One of the brightest infrared sources in our sky is the nucleus of our galaxy, only about 10 light years across. 4) This makes it a very small source for the prodigious amount of energy it emits: as much energy as radiated by 80 million Suns. 4) It also has a radio source and a variable x-ray sou ...
... 3) One of the brightest infrared sources in our sky is the nucleus of our galaxy, only about 10 light years across. 4) This makes it a very small source for the prodigious amount of energy it emits: as much energy as radiated by 80 million Suns. 4) It also has a radio source and a variable x-ray sou ...
Starlight and Atoms - School District of Clayton
... b. The upper layers of a star contain hot low-density gases that produce bright lines at precisely the same wavelengths as the dark lines, thus making them invisible. c. Hot hydrogen and helium gas in the interstellar medium produces bright lines to fill in the dark lines. d. The resolution of many ...
... b. The upper layers of a star contain hot low-density gases that produce bright lines at precisely the same wavelengths as the dark lines, thus making them invisible. c. Hot hydrogen and helium gas in the interstellar medium produces bright lines to fill in the dark lines. d. The resolution of many ...
Neutron Stars and Black Holes
... The mass of the proton is 1.67 X 10-24 g, and its radius is about 0.877 X 10-13 cm (according to the Wikipedia). The volume of the proton is 4/3 π r3 = 2.82 X 10-39 cm3. The density = mass/volume = 5.9 X 1014 g/cm3. The Sun’s mass is 2 X 1030 kg = 2 X 1033 g. A one solar mass black hole has radius r ...
... The mass of the proton is 1.67 X 10-24 g, and its radius is about 0.877 X 10-13 cm (according to the Wikipedia). The volume of the proton is 4/3 π r3 = 2.82 X 10-39 cm3. The density = mass/volume = 5.9 X 1014 g/cm3. The Sun’s mass is 2 X 1030 kg = 2 X 1033 g. A one solar mass black hole has radius r ...
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.