SRP_Space_Lesson 5 - Scientist in Residence Program
... Star, always point north and long arm of the Crux, the Southern Cross, always points south. Stars move across the night sky throughout the night, they also move ‘off’ the sky depending on the season, or might not be visible at all from a given location. This might become easier to understand if we r ...
... Star, always point north and long arm of the Crux, the Southern Cross, always points south. Stars move across the night sky throughout the night, they also move ‘off’ the sky depending on the season, or might not be visible at all from a given location. This might become easier to understand if we r ...
Placing Our Solar System in Context
... Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to proceed from inside-out as expected. ...
... Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to proceed from inside-out as expected. ...
New Astrophysical Opportunities Exploiting Spatio-Temporal Optical Correlations
... A system can be devised [6, 7] that would consist of hundreds of large flux gathering surfaces spread out over kilometers of baseline that would enable to make the next big step in astronomy: optical imaging at µ-arcsecond resolution. 2. Astrophysical applications for µ-arcsecond imaging SII Properl ...
... A system can be devised [6, 7] that would consist of hundreds of large flux gathering surfaces spread out over kilometers of baseline that would enable to make the next big step in astronomy: optical imaging at µ-arcsecond resolution. 2. Astrophysical applications for µ-arcsecond imaging SII Properl ...
Gone in a flash: supernovae in the survey era
... until carbon burning is ignited at or near its core. These are the Type Ia supernovae (SNe Ia), with distinctive features of silicon (a product of carbon burning) in the spectra. The second group forms through the gravitational core-collapse of a massive star, more than eight times the mass of the S ...
... until carbon burning is ignited at or near its core. These are the Type Ia supernovae (SNe Ia), with distinctive features of silicon (a product of carbon burning) in the spectra. The second group forms through the gravitational core-collapse of a massive star, more than eight times the mass of the S ...
Part 7
... Figure 13.1: Upper section: a schematic plot of the potential between two charged nucleons as a function of separation. At `large' separations (& 10−15 m), the repulsive Coulomb force is given by eqtn. (13.8); classically, particles cannot come closer than the point r1 at which the relative kinetic ...
... Figure 13.1: Upper section: a schematic plot of the potential between two charged nucleons as a function of separation. At `large' separations (& 10−15 m), the repulsive Coulomb force is given by eqtn. (13.8); classically, particles cannot come closer than the point r1 at which the relative kinetic ...
*Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop by Chris Hathaway and Anthony Kuchera
... One of the major, most extensively studied star-forming fields in our Galaxy is found toward the constellation Monoceros. It is located in the Northern sky, lies toward the outer parts of the Galaxy, and is thought to be part of the Perseus spiral arm of the Milky Way. It is one of the least obscure ...
... One of the major, most extensively studied star-forming fields in our Galaxy is found toward the constellation Monoceros. It is located in the Northern sky, lies toward the outer parts of the Galaxy, and is thought to be part of the Perseus spiral arm of the Milky Way. It is one of the least obscure ...
No Slide Title
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
GO 3_3 Interpreting Space
... the spectrum produced by the Sun. He noticed dark lines, called spectral lines. At the time he was unaware of what these lines were. The significance of the spectral lines was discovered about 50 years later when Kirschoff and Bunsen, two chemists, used a spectroscope to observe various chemicals ...
... the spectrum produced by the Sun. He noticed dark lines, called spectral lines. At the time he was unaware of what these lines were. The significance of the spectral lines was discovered about 50 years later when Kirschoff and Bunsen, two chemists, used a spectroscope to observe various chemicals ...
29.1 Directed Reading Guide
... _____ 55. What is the size of the sun’s core? a. 25% of 1,390 km b. 25% of 13,900 km c. 25% of 139,000 km d. 25% of 1,390,000 km 56. What is the sun’s core made up of? _______________________________________________________________ 57. How does the mass of the sun compare with the mass of Earth? ___ ...
... _____ 55. What is the size of the sun’s core? a. 25% of 1,390 km b. 25% of 13,900 km c. 25% of 139,000 km d. 25% of 1,390,000 km 56. What is the sun’s core made up of? _______________________________________________________________ 57. How does the mass of the sun compare with the mass of Earth? ___ ...
Collisions and close encounters involving massive main
... nal energy and helium fraction and constructed three-dimensional (although initially spherically symmetric) SPH models of the stars. We utilized two solar-metallicity stellar models – a 1 M star approximately halfway through its main-sequence life, and a 9 M star near the end of its main-sequence ...
... nal energy and helium fraction and constructed three-dimensional (although initially spherically symmetric) SPH models of the stars. We utilized two solar-metallicity stellar models – a 1 M star approximately halfway through its main-sequence life, and a 9 M star near the end of its main-sequence ...
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
... shown to be a valuable and simple method of organizing and classifying the stars without knowing so many other details about the stars. It has also been possible to determine the effective temperature of a number of stars from different spectral classes on the main sequence. The results gave good ag ...
... shown to be a valuable and simple method of organizing and classifying the stars without knowing so many other details about the stars. It has also been possible to determine the effective temperature of a number of stars from different spectral classes on the main sequence. The results gave good ag ...
No Slide Title
... m - M = 5 log (d/ 10pc) = 5 log (0.1” / parallax) This gave accurate distances to ~few*100 pc. ...
... m - M = 5 log (d/ 10pc) = 5 log (0.1” / parallax) This gave accurate distances to ~few*100 pc. ...
Properties of long gamma-ray bursts from massive compact binaries
... These features can also be seen in the accretion history (figure 1b). At early times, the accretion rate is only slightly lower than the single-star case, owing to the time scale for material to accrete through the disc. After roughly 104 s, the edge of the accretor’s Roche lobe prevents further mat ...
... These features can also be seen in the accretion history (figure 1b). At early times, the accretion rate is only slightly lower than the single-star case, owing to the time scale for material to accrete through the disc. After roughly 104 s, the edge of the accretor’s Roche lobe prevents further mat ...
Nuclear Physics
... A beta-minus particle b- is simply an electron that has been expelled from the nucleus. ...
... A beta-minus particle b- is simply an electron that has been expelled from the nucleus. ...
How is the Potential Energy Released
... Mass of the NS Star • In order to measure the mass of the neutron star and its optical companion we need to measure the mass function. For a circular orbit it can be shown that this is defined ...
... Mass of the NS Star • In order to measure the mass of the neutron star and its optical companion we need to measure the mass function. For a circular orbit it can be shown that this is defined ...
Type II Supernovae
... When the distance d is comparable to the stellar radius R, the neutrinos can no longer escape the star and become temporarily trapped within it. This happens when the density is about 1011−12 g/cm3 , about 1000 times less than the final neutron star density. ...
... When the distance d is comparable to the stellar radius R, the neutrinos can no longer escape the star and become temporarily trapped within it. This happens when the density is about 1011−12 g/cm3 , about 1000 times less than the final neutron star density. ...
MS Word version
... Let’s explore the boundaries of these 3 regions. Make sure you are still at a latitude of 40º N, create a star, select the long trails option for star trails, and animate for 24 hours so that a complete parallel of declination is made for the star. Now drag this active star so that it is at the nort ...
... Let’s explore the boundaries of these 3 regions. Make sure you are still at a latitude of 40º N, create a star, select the long trails option for star trails, and animate for 24 hours so that a complete parallel of declination is made for the star. Now drag this active star so that it is at the nort ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.