HR DIAGRAM REPORT FORM
... Using the enclosed graph sheets and the background handout, complete the following plots. Graphs – 10 pts each Questions – 3 pts each A. Plot an H-R diagram for the brightest stars from table 10.1. B. Plot an H-R diagram for the closest stars from table 10.2. 1. Which type of star is most common on ...
... Using the enclosed graph sheets and the background handout, complete the following plots. Graphs – 10 pts each Questions – 3 pts each A. Plot an H-R diagram for the brightest stars from table 10.1. B. Plot an H-R diagram for the closest stars from table 10.2. 1. Which type of star is most common on ...
Chapter 10 Measuring the Stars: Giants, Dwarfs, and the Main
... • Spectral class helps us determine its luminosity if it lies on the main sequence • Apply the inverse square law to determine distance Stellar Mass * ___________________________________ by looking at the common center of mass ...
... • Spectral class helps us determine its luminosity if it lies on the main sequence • Apply the inverse square law to determine distance Stellar Mass * ___________________________________ by looking at the common center of mass ...
Part 1, Some Basics
... temperature) to bottom-right (low luminosity and low surface temperature) – 90% stars in this band – The Sun is one of main sequence stars – Hydrogen burning as energy source ...
... temperature) to bottom-right (low luminosity and low surface temperature) – 90% stars in this band – The Sun is one of main sequence stars – Hydrogen burning as energy source ...
The Life Cycle of a Star and the Hertzsprung
... stars of different ages and in different stages, all at the same time. It is also a great tool to check your understanding of the star life cycle. In the Hertzsprung-Russell (HR) Diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of ...
... stars of different ages and in different stages, all at the same time. It is also a great tool to check your understanding of the star life cycle. In the Hertzsprung-Russell (HR) Diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of ...
May 2016 night sky chart
... For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown on the star chart. To use this star chart, rotate the chart so that the direct ...
... For Darwin and similar locations the chart will still apply, but some stars will be lost off the southern edge while extra stars will be visible to the north. Stars down to a brightness or magnitude limit of 4.5 are shown on the star chart. To use this star chart, rotate the chart so that the direct ...
Stellar Evolution: The Live and Death of a Star
... When burning starts and temperature increases, there is no corresponding rise in pressure, no expansion of gas & no stabilization of core The rapid temperature rise results in runaway explosion called the helium flash The helium burns ferociously for a few hours, then equilibrium is eventually re ...
... When burning starts and temperature increases, there is no corresponding rise in pressure, no expansion of gas & no stabilization of core The rapid temperature rise results in runaway explosion called the helium flash The helium burns ferociously for a few hours, then equilibrium is eventually re ...
Mass and the Properties of Main Sequence Stars
... collapse like in the case of the white dwarfs. As gravity overcomes electron degeneracy pressure, and the core collapse rapidly, the electrons and protons recombine to form neutrons, and releasing neutrinos and energy at the same time Supernova explosion. Eventually the neutron degeneracy pressure ...
... collapse like in the case of the white dwarfs. As gravity overcomes electron degeneracy pressure, and the core collapse rapidly, the electrons and protons recombine to form neutrons, and releasing neutrinos and energy at the same time Supernova explosion. Eventually the neutron degeneracy pressure ...
January 2006
... star becomes cool and opaque • solar radiation pushes it outward from the star Duration: 100,000 years Central Temperature: 300 106 K • A planetary nebula is formed Surface Temperature: 100,000 K Size: 0.1 Sun ...
... star becomes cool and opaque • solar radiation pushes it outward from the star Duration: 100,000 years Central Temperature: 300 106 K • A planetary nebula is formed Surface Temperature: 100,000 K Size: 0.1 Sun ...
Death of High Mass Stars
... • After core has a mass greater than 1.4 M (Chandrasekhar limit) the electron degeneracy is not strong enough. • Electrons are forced to combine with the protons to create neutrons. • Core collapses until pressure from physical force of neutrons bouncing against each other stops it. • Core rebounds ...
... • After core has a mass greater than 1.4 M (Chandrasekhar limit) the electron degeneracy is not strong enough. • Electrons are forced to combine with the protons to create neutrons. • Core collapses until pressure from physical force of neutrons bouncing against each other stops it. • Core rebounds ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... It was a classic case of serendipity. While investigating how supermassive black holes formed in the early universe, UC Santa Cruz postdoctoral researcher Ke-Jung Chen stumbled on the unanticipated discovery that some primordial supermassive stars could explode without leaving any black hole or othe ...
... It was a classic case of serendipity. While investigating how supermassive black holes formed in the early universe, UC Santa Cruz postdoctoral researcher Ke-Jung Chen stumbled on the unanticipated discovery that some primordial supermassive stars could explode without leaving any black hole or othe ...
lecture18
... Supernovae are so bright (10 billion times luminosity of sun) that they can be seen in very distant galaxies. The distance to the supernova tells how far away the galaxy is. ...
... Supernovae are so bright (10 billion times luminosity of sun) that they can be seen in very distant galaxies. The distance to the supernova tells how far away the galaxy is. ...
Chapter 27 Stars and Galaxies
... – Sun in 8 light minutes from Earth – Proxima Centauri: closest star to Earth (other than the sun) is 4.2 light years away Sirius (brightest star): 9 ly Polaris: 700 ly ...
... – Sun in 8 light minutes from Earth – Proxima Centauri: closest star to Earth (other than the sun) is 4.2 light years away Sirius (brightest star): 9 ly Polaris: 700 ly ...
Test 2 - Constellations - ppt
... exposure of the northern sky. The arcs are the paths of the stars circling the North Star (Polaris) in the center. These stars can be seen year-round in the northern sky although their exact location each night will vary throughout the year. ...
... exposure of the northern sky. The arcs are the paths of the stars circling the North Star (Polaris) in the center. These stars can be seen year-round in the northern sky although their exact location each night will vary throughout the year. ...
Today`s Powerpoint
... All these effects are unnoticeable in our daily experience! They are tiny in Earth’s gravity, but large in a black hole’s. ...
... All these effects are unnoticeable in our daily experience! They are tiny in Earth’s gravity, but large in a black hole’s. ...
poster
... located at 700 pc (Wilking et al. 1989). IRAS 20050+2720 displays an exceptionally low 24μm background, because no massive stars are present. This allows us to achieve a more complete sample at 24μm than in other star forming regions. We analyze Chandra observations, Spitzer, 2MASS and UBVRI photome ...
... located at 700 pc (Wilking et al. 1989). IRAS 20050+2720 displays an exceptionally low 24μm background, because no massive stars are present. This allows us to achieve a more complete sample at 24μm than in other star forming regions. We analyze Chandra observations, Spitzer, 2MASS and UBVRI photome ...
here
... • Mdust = Sν D2 / κν B(ν,T) – where Sν is the flux density, κν is the mass absorption coefficient [e.g. Hildebrand 1983] – Fits typically invoke a spectral index for the opacity, and one or two temperature components, – can have significant optical depths at λ < 60µm and may have to consider non ...
... • Mdust = Sν D2 / κν B(ν,T) – where Sν is the flux density, κν is the mass absorption coefficient [e.g. Hildebrand 1983] – Fits typically invoke a spectral index for the opacity, and one or two temperature components, – can have significant optical depths at λ < 60µm and may have to consider non ...
November | Activity of the Month
... billions of galaxies or star cities, some that are so distant it takes 10 billion years for their light to reach us in our own galaxy the Milky Way. University of Victoria’s Sara Ellison is an astronomer who is fascinated with galaxies far, far away. She uses some of the world’s newest and biggest t ...
... billions of galaxies or star cities, some that are so distant it takes 10 billion years for their light to reach us in our own galaxy the Milky Way. University of Victoria’s Sara Ellison is an astronomer who is fascinated with galaxies far, far away. She uses some of the world’s newest and biggest t ...
WEBDA - a tool for CP star research in open clusters
... in the database. The Star Clusters Young & Old Newsletter (SCYON), a bimonthly newsletter devoted to star cluster research with about 600 subscribers, is hosted in parallel with the database. Key words: Galaxy: open clusters – astronomical data bases: miscellaneous – stars: chemically peculiar ...
... in the database. The Star Clusters Young & Old Newsletter (SCYON), a bimonthly newsletter devoted to star cluster research with about 600 subscribers, is hosted in parallel with the database. Key words: Galaxy: open clusters – astronomical data bases: miscellaneous – stars: chemically peculiar ...
ASTR2050 Spring 2005 •
... White light breaks up into colors, but that’s only a small part of the story. ...
... White light breaks up into colors, but that’s only a small part of the story. ...
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.