Stars and The Universe
... for non-majors in mathematics or a physical science. A companion science lab, Astronomy 30, is also available. 3 hours. [Typical contact hours: 52.5] Prerequisite Skills: None Expected Outcomes for Students: Upon completion of the course, the student should be able to: ...
... for non-majors in mathematics or a physical science. A companion science lab, Astronomy 30, is also available. 3 hours. [Typical contact hours: 52.5] Prerequisite Skills: None Expected Outcomes for Students: Upon completion of the course, the student should be able to: ...
Stellar Evolution after the Main Sequence
... What's Left… • After the massive star implodes (followed by the supernova explosion) the inner part of the star remains. • If the mass of this inner core is less than about 4 solar masses then it becomes stable. • What's left is about the size of Manhattan Island (with up to 4 times the mass of the ...
... What's Left… • After the massive star implodes (followed by the supernova explosion) the inner part of the star remains. • If the mass of this inner core is less than about 4 solar masses then it becomes stable. • What's left is about the size of Manhattan Island (with up to 4 times the mass of the ...
Tools of Modern Astronomy Slide Show
... 9. The Earth’s _______________ distorts EM radiation. UV, x-ray, & gamma ray telescopes are placed on _____________ for best “seeing”. The _____________ is the best visible light telescope because it is above the atmosphere. 10. Astronomers use _______________ to collect chemical composition and tem ...
... 9. The Earth’s _______________ distorts EM radiation. UV, x-ray, & gamma ray telescopes are placed on _____________ for best “seeing”. The _____________ is the best visible light telescope because it is above the atmosphere. 10. Astronomers use _______________ to collect chemical composition and tem ...
1201 Discussion Notes
... Remember, the orbits in an elliptical galaxy are fairly random, so even if we focus on one area there will be a range of Doppler shifted lines from the stars that are moving towards and away from us at different speeds. These all combine (they sort of add together) to make a broadened line. The broa ...
... Remember, the orbits in an elliptical galaxy are fairly random, so even if we focus on one area there will be a range of Doppler shifted lines from the stars that are moving towards and away from us at different speeds. These all combine (they sort of add together) to make a broadened line. The broa ...
Lesson 2 | The Sun and Other Stars
... Key Concept How are stars layered? Directions: Use the diagram to respond to each statement on the lines provided. ...
... Key Concept How are stars layered? Directions: Use the diagram to respond to each statement on the lines provided. ...
THE BIG BANG - Dublin City Schools
... • Singularity: The theory is that one single finite speck (much much smaller than a pin head) with extremely high density and temperature instantly started expanding and inflating. (like the surface of an inflated balloon) ...
... • Singularity: The theory is that one single finite speck (much much smaller than a pin head) with extremely high density and temperature instantly started expanding and inflating. (like the surface of an inflated balloon) ...
slides
... The central core (which, in the most massive stars, is made of iron) undergoes a sudden gravitational collapse, reducing in size until all the electrons in the atoms are smashed down into the nulcei. ...
... The central core (which, in the most massive stars, is made of iron) undergoes a sudden gravitational collapse, reducing in size until all the electrons in the atoms are smashed down into the nulcei. ...
STAAR Review – Week Ten
... 12. In the center of the Milky Way is a large bulge of stars. Within this bulge lies a black hole. The Sun is located – a. outside of the Milky Way. b. in the large bulge of stars near the center of the Milky Way. c. in the black hole in the center of the Milky Way. d. near the edge of the Milky Way ...
... 12. In the center of the Milky Way is a large bulge of stars. Within this bulge lies a black hole. The Sun is located – a. outside of the Milky Way. b. in the large bulge of stars near the center of the Milky Way. c. in the black hole in the center of the Milky Way. d. near the edge of the Milky Way ...
PPT file
... in PRAO. It’s the most long set observations. 125 sources are in the modern list for observation once in the month. Here two type sources: super compact (~1au) gaze clouds in star formation regions and envelopes of variable late spectra classes stars. In star formation regions was found periodicity ...
... in PRAO. It’s the most long set observations. 125 sources are in the modern list for observation once in the month. Here two type sources: super compact (~1au) gaze clouds in star formation regions and envelopes of variable late spectra classes stars. In star formation regions was found periodicity ...
4550-15Lecture35
... ephemeral streams now. To attain the necessary temperatures, Mars must have had CO2 pressures at its surface of 5 to 10 atm. This early atmosphere has been lost, a consequence of lower gravity and the lack of a geomagnetic field that prevents erosion of the atmosphere by the solar wind. Thus the dep ...
... ephemeral streams now. To attain the necessary temperatures, Mars must have had CO2 pressures at its surface of 5 to 10 atm. This early atmosphere has been lost, a consequence of lower gravity and the lack of a geomagnetic field that prevents erosion of the atmosphere by the solar wind. Thus the dep ...
Chapter 14
... If the stellar core has more than three solar masses after supernova, then no known force can halt the collapse ...
... If the stellar core has more than three solar masses after supernova, then no known force can halt the collapse ...
The Hertzsprung-Russell Diagram
... star against its spectral type. This works best for a cluster, where you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
... star against its spectral type. This works best for a cluster, where you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
The Stellar Cycle
... • The core implodes, but no fuel there, so it collapses until neutron degeneracy pressure kicks in. • Core “bounces” when it hits neutron limit; huge neutrino release; unspent fuel outside core fuses… ...
... • The core implodes, but no fuel there, so it collapses until neutron degeneracy pressure kicks in. • Core “bounces” when it hits neutron limit; huge neutrino release; unspent fuel outside core fuses… ...
1 - Stellar Life Cycle
... it's all over, a large fraction of the star is blown into space as a supernova remnant. A typical supernova remnant is at most few light-years across. (M 1 shown) ...
... it's all over, a large fraction of the star is blown into space as a supernova remnant. A typical supernova remnant is at most few light-years across. (M 1 shown) ...
Star Groups and Big Bang Power Point
... Hubble determined the speed at which the galaxies were moving away from Earth. Hubble found that the most distant galaxies showed the greatest red shift and thus were moving away from Earth the fastest. ...
... Hubble determined the speed at which the galaxies were moving away from Earth. Hubble found that the most distant galaxies showed the greatest red shift and thus were moving away from Earth the fastest. ...
Stellar Evolution
... How does mass affect what happens? How do stars die? Where does gold come from? ...
... How does mass affect what happens? How do stars die? Where does gold come from? ...
Lecture 6-1: Schematic Evolution of Stars as seen from the core
... increase to support the star against gravity. As thermal pressure scales with r while hydrostatic pressure scales with r4/3, a more massive star requires a higher central temperature (and/or lower density). For a non-relativistic degenerate gas, temperature doesn’t enter. Now, thermal pressure scale ...
... increase to support the star against gravity. As thermal pressure scales with r while hydrostatic pressure scales with r4/3, a more massive star requires a higher central temperature (and/or lower density). For a non-relativistic degenerate gas, temperature doesn’t enter. Now, thermal pressure scale ...
From studying our solar system to searching for worlds beyond and
... and how quickly they move.” This European Space Agency spacecraft is scheduled to launch later this year, and Belokurov has big plans for its data: “As I look at the stars torn off other celestial bodies as they now travel around the Milky Way, I plan to study the shape and lumpiness of the gravitat ...
... and how quickly they move.” This European Space Agency spacecraft is scheduled to launch later this year, and Belokurov has big plans for its data: “As I look at the stars torn off other celestial bodies as they now travel around the Milky Way, I plan to study the shape and lumpiness of the gravitat ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
... The evolution of massive stars have the following general characteristics and differences to lower mass evolution 1. The electrons in their cores do not become degenerate until the final burning stages, when iron core is reached 2. Mass-loss plays an important role in the entire evolution (we will c ...
L11
... The convective core becomes exhausted homogeneously, while it contracts to a smaller volume and becomes hotter. The star also develops a H-burning shell around the He dominated core. The temperature at the bottom of the hydrogen envelope is too high to sustain hydrostatic equilibrium. The envelope e ...
... The convective core becomes exhausted homogeneously, while it contracts to a smaller volume and becomes hotter. The star also develops a H-burning shell around the He dominated core. The temperature at the bottom of the hydrogen envelope is too high to sustain hydrostatic equilibrium. The envelope e ...
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.