22/06/2016 - Daphne`s Daily Quiz
... 13. Which fish in the genus Zeus, has a dark spot on either side of its body, and is also known as St Pierre? 14. In Norse mythology, what name is given to the golden arm ring, belonging to Odin, which spawned eight new rings every ninth day? 15. How is port, aged for many years in a cask, rather th ...
... 13. Which fish in the genus Zeus, has a dark spot on either side of its body, and is also known as St Pierre? 14. In Norse mythology, what name is given to the golden arm ring, belonging to Odin, which spawned eight new rings every ninth day? 15. How is port, aged for many years in a cask, rather th ...
The Milky Way
... How can we measure the mass of the Milky Way? Why do stars behind dust clouds appear red? Why is the sky blue? Why are wavelengths of light outside the visible useful in studying the Milky Way? • How is the 21 cm line of Hydrogen produced? • Describe the spiral arms of the Milky Way and what ...
... How can we measure the mass of the Milky Way? Why do stars behind dust clouds appear red? Why is the sky blue? Why are wavelengths of light outside the visible useful in studying the Milky Way? • How is the 21 cm line of Hydrogen produced? • Describe the spiral arms of the Milky Way and what ...
X-ray binaries
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
X-ray binaries
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
Population synthesis view of gravitational waves - Astro-PF
... sources from the model Obtain galactic merger rate Extrapolate from the Galaxy further out: Scale by: mass density? galaxy density? blue luminosity? Supernovae rate density? ...
... sources from the model Obtain galactic merger rate Extrapolate from the Galaxy further out: Scale by: mass density? galaxy density? blue luminosity? Supernovae rate density? ...
shirley - Yancy L. Shirley`s Webpage
... How do you form a star with M > 10 Msun before radiation pressure stops accretion? ...
... How do you form a star with M > 10 Msun before radiation pressure stops accretion? ...
The Transit Method
... de France. The sky was clear but he could not make measurements due to the motion of the ship. Coming this far he decided to just wait for the next transit in 8 years. He then mapped the eastern coast of Madagascar and decided to observe the second transit from Manilla in the Philippines. The Spanis ...
... de France. The sky was clear but he could not make measurements due to the motion of the ship. Coming this far he decided to just wait for the next transit in 8 years. He then mapped the eastern coast of Madagascar and decided to observe the second transit from Manilla in the Philippines. The Spanis ...
Widener University
... c) Calculate the Roche limit for a small frozen moon composed of water ice ( = 1000 kg/m3) near this ...
... c) Calculate the Roche limit for a small frozen moon composed of water ice ( = 1000 kg/m3) near this ...
Supplementary Information
... Figure S3. λ=6583 [NII] and line free K-band continuum maps of BzK-15504, compared to Hα. Panels a-e are from the 0.125”x0.25” pixel data set (FWHM resolution 0.45”, indicated by shaded circles at the bottom right of each map). Panel f is from the high resolution data set (smoothed to 0.23” FWHM), w ...
... Figure S3. λ=6583 [NII] and line free K-band continuum maps of BzK-15504, compared to Hα. Panels a-e are from the 0.125”x0.25” pixel data set (FWHM resolution 0.45”, indicated by shaded circles at the bottom right of each map). Panel f is from the high resolution data set (smoothed to 0.23” FWHM), w ...
Understanding Stars
... stars, and add these values to the temperature-luminosity diagram on the board. The accompanying handout gives recipes for calculating, in physical units, the properties of any star based only on its spectrum, apparent brightness, and parallax. However, we'd rather not have to deal with loads of con ...
... stars, and add these values to the temperature-luminosity diagram on the board. The accompanying handout gives recipes for calculating, in physical units, the properties of any star based only on its spectrum, apparent brightness, and parallax. However, we'd rather not have to deal with loads of con ...
ASTRO-114--Lecture 40-
... It’s the size of the distances between the stars. And this cloud has stars forming in it. And in the upper right drawing — or picture; it’s actually a photograph — you see an arrow pointing at a couple of very bright stars that have just recently formed in this cloud. Now, here are a couple of color ...
... It’s the size of the distances between the stars. And this cloud has stars forming in it. And in the upper right drawing — or picture; it’s actually a photograph — you see an arrow pointing at a couple of very bright stars that have just recently formed in this cloud. Now, here are a couple of color ...
Chapter 6: Stellar Evolution (part 2)
... I But, physically most of the accreted materials is fused to carbon and oxygen during nova and possibly ejected. So all these need to lead to the increase of the WD mass. I The accumulated X-ray emission from such accreting sources, as observed from nearby galaxies, seems to be far less than require ...
... I But, physically most of the accreted materials is fused to carbon and oxygen during nova and possibly ejected. So all these need to lead to the increase of the WD mass. I The accumulated X-ray emission from such accreting sources, as observed from nearby galaxies, seems to be far less than require ...
PowerPoint
... • These are objects that are below 80 Jupiter masses. • The central density and temperature do not get large enough for nuclear fusion to occur. • These failed stars, gradually cool down and contract. • Recently, there have been a number of discovered brown dwarves. ...
... • These are objects that are below 80 Jupiter masses. • The central density and temperature do not get large enough for nuclear fusion to occur. • These failed stars, gradually cool down and contract. • Recently, there have been a number of discovered brown dwarves. ...
High-Speed Ballistic Stellar Interlopers
... approach between two binary star systems—or a binary system and a third star. In such cases, one or more of the stars can pick up enough energy through gravitational interaction with the others to be thrown from the system. Determining how many stars have been ejected from their neighbors is importa ...
... approach between two binary star systems—or a binary system and a third star. In such cases, one or more of the stars can pick up enough energy through gravitational interaction with the others to be thrown from the system. Determining how many stars have been ejected from their neighbors is importa ...
The University of Sydney Page
... Very low mass stars Very low mass stars (mass less than about 0.4 solar masses) are different in one important respect from heavier stars: their interiors are fully convective. The fused helium is stirred through the whole star, so it has the whole of its hydrogen mass to prolong its stay on the ma ...
... Very low mass stars Very low mass stars (mass less than about 0.4 solar masses) are different in one important respect from heavier stars: their interiors are fully convective. The fused helium is stirred through the whole star, so it has the whole of its hydrogen mass to prolong its stay on the ma ...
PowerPoint Presentation - Center for Gravitational Wave Physics
... He burning is thermally stable when donor mass is 0.2-0.27, with orbital periods of 2.5-3.5 minutes (Tutukov & Yungelson ‘96). As the accretion rate drops, the burning becomes unstable, and flashes ...
... He burning is thermally stable when donor mass is 0.2-0.27, with orbital periods of 2.5-3.5 minutes (Tutukov & Yungelson ‘96). As the accretion rate drops, the burning becomes unstable, and flashes ...
Unit 11: Stellar Evolution
... the neutrinos being radiated away from the core. In a fraction of a second, the earthsized iron core is transformed into a neutron core about 10 miles across. The unsupported outer regions are now free-falling toward the neutron core. The implosion is converted into an explosion by a combination of ...
... the neutrinos being radiated away from the core. In a fraction of a second, the earthsized iron core is transformed into a neutron core about 10 miles across. The unsupported outer regions are now free-falling toward the neutron core. The implosion is converted into an explosion by a combination of ...
hubble_refurb
... decision, and would consider sending a shuttle to repair Hubble.[Zimmerman 2] As an engineer, Griffin had previously worked on Hubble's construction, and respected the discoveries the telescope brought to the science community.[Zimmerman 2] He agreed with the National Academy of Sciences that a robo ...
... decision, and would consider sending a shuttle to repair Hubble.[Zimmerman 2] As an engineer, Griffin had previously worked on Hubble's construction, and respected the discoveries the telescope brought to the science community.[Zimmerman 2] He agreed with the National Academy of Sciences that a robo ...
Untitled - Notion Press
... gravity at this point becomes such intense that not even light can escape from its gravitational force. This is a black hole. These stars of the mass of more than 8 to 20 times of solar mass end with a ‘supernova.’ The stars of these masses leave superheated plasma during supernova. The energy of th ...
... gravity at this point becomes such intense that not even light can escape from its gravitational force. This is a black hole. These stars of the mass of more than 8 to 20 times of solar mass end with a ‘supernova.’ The stars of these masses leave superheated plasma during supernova. The energy of th ...
Chapter 14 – Chemical Analysis
... the COG for Weak Lines • Both the ionization equilibrium and the opacity depend on surface gravity • For neutral lines of ionized species (e.g. Fe I in the Sun) these effects cancel, so the COG is independent of gravity • For ionized lines of ionized species (e.g Fe II in the Sun), the curves shift ...
... the COG for Weak Lines • Both the ionization equilibrium and the opacity depend on surface gravity • For neutral lines of ionized species (e.g. Fe I in the Sun) these effects cancel, so the COG is independent of gravity • For ionized lines of ionized species (e.g Fe II in the Sun), the curves shift ...
ANTARES - National Optical Astronomy Observatory
... different algorithms used to determine the credible region. The total area is greater than 600 square degrees while follow-up images on the ground generally have a field-of-view of less than one square degree. Figure from Abbott et al. (2016b). will be annotated in the alert. Such galaxy catalogs do ...
... different algorithms used to determine the credible region. The total area is greater than 600 square degrees while follow-up images on the ground generally have a field-of-view of less than one square degree. Figure from Abbott et al. (2016b). will be annotated in the alert. Such galaxy catalogs do ...
astrocoursespring2012lec4
... not only the universe today, but also the universe in the past. Using modern telescopes and computers, astronomers have studied numerous properties of globular clusters. Here are just some of the quantities that we can measure for globular clusters: •size (radius), •mass, •distance from galactic cen ...
... not only the universe today, but also the universe in the past. Using modern telescopes and computers, astronomers have studied numerous properties of globular clusters. Here are just some of the quantities that we can measure for globular clusters: •size (radius), •mass, •distance from galactic cen ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.