The basic physical properties of a star Hydrostatic equilibrium
... • Energy generation in stars • Energy transport ...
... • Energy generation in stars • Energy transport ...
H-R diagram worksheet
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
... Mark each of the following on the H-R diagram and label it as indicated. You may use page 15 of your ESRT to help you. 6. Draw and label a long diagonal line showing the approximate location of the main sequence. 7. A large circle indicating the area where you find the biggest diameter stars, labele ...
ppt
... Thanks to the water-ice and rocky material, Jupiter grew fast. When Jupiter’s core reached 10-15 M, its gravitational influence is strong enough to form its own accretion disk. ...
... Thanks to the water-ice and rocky material, Jupiter grew fast. When Jupiter’s core reached 10-15 M, its gravitational influence is strong enough to form its own accretion disk. ...
Stars
... • Apparent Magnitude – How bright the star really looks from Earth. The farther away from us, the dimmer the star looks. • Absolute Magnitude – How bright the star really is. If all stars were the same distance from us, how bright would it look compared to the other ...
... • Apparent Magnitude – How bright the star really looks from Earth. The farther away from us, the dimmer the star looks. • Absolute Magnitude – How bright the star really is. If all stars were the same distance from us, how bright would it look compared to the other ...
Properties of Stars - Mr. Carter`s Earth
... • The brightest moment is seen within a few days, remains bright for a few weeks, then returns to normal brightness within a year. _______________________ (interstellar matter): clouds of dust and gases. – If this matter gets too close to a hot star, it will ____________________. – This is known as ...
... • The brightest moment is seen within a few days, remains bright for a few weeks, then returns to normal brightness within a year. _______________________ (interstellar matter): clouds of dust and gases. – If this matter gets too close to a hot star, it will ____________________. – This is known as ...
Russell Diagram
... massive as the other. They are 2.0 AU apart and have an orbit period of 0.50 y. What is the mass of the smaller star in terms of solar masses? ...
... massive as the other. They are 2.0 AU apart and have an orbit period of 0.50 y. What is the mass of the smaller star in terms of solar masses? ...
Hertzsprung-Russell Diagram
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
... A star has a high luminosity (100 solar luminosities) and a surface temperature of 3500 K. What type of star is it? ...
Stages 12 to 14
... The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too small, the ignition temperatu ...
... The carbon rich core continues to contract and heat up. Carbon fusion requires a temperature of 500 to 600 million K. The core will contract until electron degeneracy pressure once again takes over, and contraction ends If the star is similar to the sun, the mass is too small, the ignition temperatu ...
Nuclear Interactions in Supernovae .
... • Stars undergo nuclear fusion within their cores in order to keep themselves alive. • A star is in a constant state of thermal equilibrium with itself, perfectly balancing out the crushing gravitational force from its massive core and the continuously exploding outward pressure from its nuclear rea ...
... • Stars undergo nuclear fusion within their cores in order to keep themselves alive. • A star is in a constant state of thermal equilibrium with itself, perfectly balancing out the crushing gravitational force from its massive core and the continuously exploding outward pressure from its nuclear rea ...
Before Reading
... How Many Stars in the Sky? • What are the problems the child encounters trying to count the stars in the sky? • Why is the country a better place than the city to see stars? • Do you think it is possible to count all the stars in the sky? Why or why not? ...
... How Many Stars in the Sky? • What are the problems the child encounters trying to count the stars in the sky? • Why is the country a better place than the city to see stars? • Do you think it is possible to count all the stars in the sky? Why or why not? ...
Quiz Solution: 1 April 2013 What does it mean when an astronomer
... Quiz Solution: 1 April 2013 What does it mean when an astronomer says that a star "moves" from one place to another on an H-R Diagram? Can you provide an example of this? As stars evolve and change structure, their radii and temperatures also change. Since a star's luminosity is dependent on both te ...
... Quiz Solution: 1 April 2013 What does it mean when an astronomer says that a star "moves" from one place to another on an H-R Diagram? Can you provide an example of this? As stars evolve and change structure, their radii and temperatures also change. Since a star's luminosity is dependent on both te ...
Name________________ Astronomy I cans 1. What is the Big Bang
... When atoms combine and create heat and light A nuclear fusion reaction causes the nuclei of an atom to gain more protons and release energy. Energy (heat and light) The core of stars Nuclear fusion fuses heavier atoms together to create even heavier atoms on the Periodic Table ...
... When atoms combine and create heat and light A nuclear fusion reaction causes the nuclei of an atom to gain more protons and release energy. Energy (heat and light) The core of stars Nuclear fusion fuses heavier atoms together to create even heavier atoms on the Periodic Table ...
Day-7
... Method is robust but you must be patient: Require at least 3 transits, preferably 4 with same brightness change, duration and temporal separation (the first two establish a possible period, the third confirms it) ...
... Method is robust but you must be patient: Require at least 3 transits, preferably 4 with same brightness change, duration and temporal separation (the first two establish a possible period, the third confirms it) ...
jackie822 beanerbutt777 life cycle of a star
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
... http://solarsystem.nasa.gov/multimedia/gallery/prominence.gif ...
Today`s Powerpoint
... If a star is moving rapidly towards Earth then its spectrum will be: A: the same as if it were at rest B: shifted to the blue C: shifted to the red D: much brighter than if it were at rest E: much fainter than if it were at rest ...
... If a star is moving rapidly towards Earth then its spectrum will be: A: the same as if it were at rest B: shifted to the blue C: shifted to the red D: much brighter than if it were at rest E: much fainter than if it were at rest ...
Lesson 10 Red Shift
... energy). Although the electromagnetic spectrum comprises wavelengths from ultra high energy (and dangerous) gamma rays to ultra low energy radio waves, the only part that we can see is the very limited "visual spectrum." In the visual spectrum, wavelength corresponds to colour. In other words, viole ...
... energy). Although the electromagnetic spectrum comprises wavelengths from ultra high energy (and dangerous) gamma rays to ultra low energy radio waves, the only part that we can see is the very limited "visual spectrum." In the visual spectrum, wavelength corresponds to colour. In other words, viole ...
Chandra and NIR Observations of Galactic HII Regions
... Massive Stars in M16 • The 11 O5 V - O9.5 V stars in NGC 6611 are all detected with Chandra, with LX in the range 5.3´1030 – 1.8x1032 ergs s-1, LX/Lbol in the range 1.4x10-8 – 6.8x10-8, and kT from 0.49–0.96 keV. • The 2-Myr old O stars in NGC 6611 have relatively soft X-ray spectra and low LX/Lbol ...
... Massive Stars in M16 • The 11 O5 V - O9.5 V stars in NGC 6611 are all detected with Chandra, with LX in the range 5.3´1030 – 1.8x1032 ergs s-1, LX/Lbol in the range 1.4x10-8 – 6.8x10-8, and kT from 0.49–0.96 keV. • The 2-Myr old O stars in NGC 6611 have relatively soft X-ray spectra and low LX/Lbol ...
Powerpoint
... Why is the gas ionized? Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are form ...
... Why is the gas ionized? Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are form ...
Time From the Perspective of a Particle Physicist
... are remnants from the first few minutes after the Big Bang • To explore back to earlier times we use our understanding of physics • The earlier you go in time the hotter was the Universe. Particle accelerators can ...
... are remnants from the first few minutes after the Big Bang • To explore back to earlier times we use our understanding of physics • The earlier you go in time the hotter was the Universe. Particle accelerators can ...
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.