Chapter 16 Galaxies and Dark Matter
... large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another galaxy, perhaps one of those on the right. ...
... large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another galaxy, perhaps one of those on the right. ...
2009 Assessment Schedule (90764)
... Explains that spectra are directly related to atomic structures. Thus hydrogen and helium will show the spectral characteristics unique to hydrogen and helium. (m) ...
... Explains that spectra are directly related to atomic structures. Thus hydrogen and helium will show the spectral characteristics unique to hydrogen and helium. (m) ...
Transcript_Forbidden Planets
... still manage to deliver lethal doses of high energy radiation onto the planet – and probably generate enough solar wind to blow away the atmosphere – and they would only last of few million years before going supernova, which would be insufficient time for the indigenous Tatooine life-forms to have ...
... still manage to deliver lethal doses of high energy radiation onto the planet – and probably generate enough solar wind to blow away the atmosphere – and they would only last of few million years before going supernova, which would be insufficient time for the indigenous Tatooine life-forms to have ...
PHY299B Poster-Justin Hudson-v2
... pictures. • With this done, we type in the coordinates to the target star. We must use the star map to find the target star, center it, then set a series of pictures over time and let the telescope collect our data. ...
... pictures. • With this done, we type in the coordinates to the target star. We must use the star map to find the target star, center it, then set a series of pictures over time and let the telescope collect our data. ...
(AU): Average distance from Earth to Sun
... Iron core of a high-mass star continues to collapse and becomes a super-dense Neutron Star. A teaspoon weighs 10 million tons! BUT iron core of a very-high-mass star collapses further and becomes … a Black Hole. ...
... Iron core of a high-mass star continues to collapse and becomes a super-dense Neutron Star. A teaspoon weighs 10 million tons! BUT iron core of a very-high-mass star collapses further and becomes … a Black Hole. ...
The Sun PPT
... • The diameter of the Sun is thus 109 times as great as the Earth's diameter. • About 1.3 million Earths could fit inside the sun. • The mass of the sun is 1.989 x 1030kilograms, about 332,000 times the mass of the Earth. • Volume of the Sun is about 1.5 million times that of Earth’s • Mean density ...
... • The diameter of the Sun is thus 109 times as great as the Earth's diameter. • About 1.3 million Earths could fit inside the sun. • The mass of the sun is 1.989 x 1030kilograms, about 332,000 times the mass of the Earth. • Volume of the Sun is about 1.5 million times that of Earth’s • Mean density ...
Scientists Observe Star Triplets Being Born : Space
... multiple-star system. Scientists suspected that the process was casused by a gravitational instability, but new observations from the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA) showed the process in action. John Tobin, from the University of Okl ...
... multiple-star system. Scientists suspected that the process was casused by a gravitational instability, but new observations from the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA) showed the process in action. John Tobin, from the University of Okl ...
Astroparticle physics 1. stellar astrophysics and solar neutrinos
... Stellar classification • Spectroscopic lines need for spectral classification. • Types OBAFGKM temperature sequence. ...
... Stellar classification • Spectroscopic lines need for spectral classification. • Types OBAFGKM temperature sequence. ...
Evolved massive stars in W33 and in GMC G23.3-0.3
... and at the parallactic distance of 2.4 kpc (Immer et al. 2013). We spectroscopically detected a few evolved O-type stars and one Wolf-Rayet star, but none of the late-type objects has the luminosity of a RSG star. Several dense molecular cores that may harbor proto clusters were recently discovered ...
... and at the parallactic distance of 2.4 kpc (Immer et al. 2013). We spectroscopically detected a few evolved O-type stars and one Wolf-Rayet star, but none of the late-type objects has the luminosity of a RSG star. Several dense molecular cores that may harbor proto clusters were recently discovered ...
Lesson 4, Stars
... Objectives Define some of the properties of stars. Compare the evolutionary paths of star ...
... Objectives Define some of the properties of stars. Compare the evolutionary paths of star ...
Discrimination of exoplanetary and stellar radio flux
... The slowly varying component does not contribute in the frequency range relevant for Jupiter’s emission, and changes on a relatively slow timescale. Noise storms Noise storms could be a problem for more active stars (or weak planetary emissions, but then detection is much more the problem than discr ...
... The slowly varying component does not contribute in the frequency range relevant for Jupiter’s emission, and changes on a relatively slow timescale. Noise storms Noise storms could be a problem for more active stars (or weak planetary emissions, but then detection is much more the problem than discr ...
Paul Green - Chandra X-Ray Observatory (CXC)
... In 1962, Scorpius X-1 became the first X-ray source discovered outside the Solar System. In the 50 years since, X-ray binaries have proven to be important for studies of fundamental physical processes such as mass accretion and jet formation. Contemporary X-ray satellites provide detailed spectrosco ...
... In 1962, Scorpius X-1 became the first X-ray source discovered outside the Solar System. In the 50 years since, X-ray binaries have proven to be important for studies of fundamental physical processes such as mass accretion and jet formation. Contemporary X-ray satellites provide detailed spectrosco ...
journey to the stars - American Museum of Natural History
... It brightens our days, providing us with more light and energy than all the stars in the night sky combined. It isn’t the brightest star out there, and it isn’t the hottest. But it’s the closest star to Earth…the star we need to ...
... It brightens our days, providing us with more light and energy than all the stars in the night sky combined. It isn’t the brightest star out there, and it isn’t the hottest. But it’s the closest star to Earth…the star we need to ...
Scientists classify stars by
... Distance makes them look different. The same is true for stars. Two stars could be the same brightness but their distance from us makes their brightness different. ...
... Distance makes them look different. The same is true for stars. Two stars could be the same brightness but their distance from us makes their brightness different. ...
H-R Diagram - Faculty Website Listing
... Please read the section in textbook that talks about HR diagram. We have also discussed this in class with examples. It may be useful to have your class notes with you when you do the lab. You can also look them up on the class webpage. 1. Using Stellarium software to collect the information on abso ...
... Please read the section in textbook that talks about HR diagram. We have also discussed this in class with examples. It may be useful to have your class notes with you when you do the lab. You can also look them up on the class webpage. 1. Using Stellarium software to collect the information on abso ...
![[WC 6] nucleus with other emission-lines nuclei of planetary nebulae](http://s1.studyres.com/store/data/004159324_1-0806f9baff29e598ec0946db112c7fad-300x300.png)
[WC 6] nucleus with other emission-lines nuclei of planetary nebulae
... 3.3. Physical parameters M 1-25. From our 1993 spectra, and from high resolution spectra taken with the 1.4m of the ESO in the framework of an other program (devoted to expansion velocities of the galactic bulge PN, see Acker, 1993), we have calculated the following parameters for M 1-25 : T of the ...
... 3.3. Physical parameters M 1-25. From our 1993 spectra, and from high resolution spectra taken with the 1.4m of the ESO in the framework of an other program (devoted to expansion velocities of the galactic bulge PN, see Acker, 1993), we have calculated the following parameters for M 1-25 : T of the ...
26Masses - NMSU Astronomy
... A. Planet A will move faster because the gravitational pull from the star is bigger on planet A B. Planet B will move faster because the gravitational pull from the star is bigger on planet B C. Both planets A and B should be moving at the same speed because the gravitational pulls are the same, bec ...
... A. Planet A will move faster because the gravitational pull from the star is bigger on planet A B. Planet B will move faster because the gravitational pull from the star is bigger on planet B C. Both planets A and B should be moving at the same speed because the gravitational pulls are the same, bec ...
Astronomy MCAS Questions Multiple Choice 1.) The diagram below
... a. Name two types of eclipses that involve the Sun, the Moon, and Earth. b. Identify the phase of the Moon during each type of eclipse you named in part (a). c. Choose one of the types of eclipses that you named in part (a) and describe (or draw a diagram that shows) the relative positions of the Su ...
... a. Name two types of eclipses that involve the Sun, the Moon, and Earth. b. Identify the phase of the Moon during each type of eclipse you named in part (a). c. Choose one of the types of eclipses that you named in part (a) and describe (or draw a diagram that shows) the relative positions of the Su ...
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.