Chapter 8, Lesson 4, 2nd Packet, pdf
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
... Compare the development of a less-massive star with that of a more-massive star. ___________________________________________________________________ ___________________________________________________________________ ___________________________________________________________________ _______________ ...
astr study guide ex 3 s`16
... How much of the average star’s lifetime is spend on the main sequence? 10. What causes the outward gas pressure that balances the inward pull of gravity in a main sequence star? 11. What is the lifetime of a 10 solar mass star on the main sequence? Estimate using table 9-2 12. What is the lifetime o ...
... How much of the average star’s lifetime is spend on the main sequence? 10. What causes the outward gas pressure that balances the inward pull of gravity in a main sequence star? 11. What is the lifetime of a 10 solar mass star on the main sequence? Estimate using table 9-2 12. What is the lifetime o ...
Galaxy Notes Presentation
... number of stars in the galaxy, can estimate as roughly 100 billion ...
... number of stars in the galaxy, can estimate as roughly 100 billion ...
File
... crust, about a kilometer thick. This crust is very hard and very smooth. Gravity would probably prevent any irregularities larger than half a centimeter. ...
... crust, about a kilometer thick. This crust is very hard and very smooth. Gravity would probably prevent any irregularities larger than half a centimeter. ...
April11
... • Iron cannot be fused into any heavier element, so it collects at the center of the star • Gravity pulls the core of the star to a size smaller than the Earth’s diameter! • The core compresses so much that protons and electrons merge into neutrons, taking energy away from the core • The core collap ...
... • Iron cannot be fused into any heavier element, so it collects at the center of the star • Gravity pulls the core of the star to a size smaller than the Earth’s diameter! • The core compresses so much that protons and electrons merge into neutrons, taking energy away from the core • The core collap ...
How the Universe Works Extreme Stars Name 1. When a star dies
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
here
... 1: Red dwarf (e.g., an M star) implies low-mass. Low-metallicity implies Pop II. Perpendicular through the disk implies not a disk-like orbit. Thus, this is likely an old, Pop II star from the stellar halo of the Milky Way. 2: Before Big Bang Nucleosynthesis, the universe was too hot for nuclei like ...
... 1: Red dwarf (e.g., an M star) implies low-mass. Low-metallicity implies Pop II. Perpendicular through the disk implies not a disk-like orbit. Thus, this is likely an old, Pop II star from the stellar halo of the Milky Way. 2: Before Big Bang Nucleosynthesis, the universe was too hot for nuclei like ...
PowerPoint File
... What do we see at the galactic center (radio and infrared wavelengths? • Strong radio source (synchrotron radiation) • At infrared wavelengths, can see stars orbiting very vast around Sgr A • http://antwrp.gsfc.nasa.gov/apod/ap001220. html • Ten years of observations speeded up ...
... What do we see at the galactic center (radio and infrared wavelengths? • Strong radio source (synchrotron radiation) • At infrared wavelengths, can see stars orbiting very vast around Sgr A • http://antwrp.gsfc.nasa.gov/apod/ap001220. html • Ten years of observations speeded up ...
PS 224, Fall 2014 HW 4
... a: Dark cloud: Large molecular clouds develop dense regions that appear darker than surrounding regions. This can be precipitated by external pressure or forces or random fluctuations present in the cloud. These regions are very large, typically around 200,000 AU. b: Gravitational collapse: When the ...
... a: Dark cloud: Large molecular clouds develop dense regions that appear darker than surrounding regions. This can be precipitated by external pressure or forces or random fluctuations present in the cloud. These regions are very large, typically around 200,000 AU. b: Gravitational collapse: When the ...
– 1 – 1. Star Formation At Low Metallicity 1.1.
... Fig. 2.— Objects cool when tc << tf f < H −1 , where tc is the cooling time, tf f is the free fall time, H −1 is the expansion timescale of the universe. The lower right shaded area corresponds to regions where TCM B > Tvir , the virial temperature. Such regions cannot cool at all irrespective of th ...
... Fig. 2.— Objects cool when tc << tf f < H −1 , where tc is the cooling time, tf f is the free fall time, H −1 is the expansion timescale of the universe. The lower right shaded area corresponds to regions where TCM B > Tvir , the virial temperature. Such regions cannot cool at all irrespective of th ...
Universe 8e Lecture Chapter 17 Nature of Stars
... mass less than 3 M, a magnetic field 1012 times stronger than that of the Sun, and a rotation period of roughly 1 second. Pulsars: A pulsar is a source of periodic pulses of radio radiation. These pulses are produced as beams of radio waves from a neutron star’s magnetic poles sweep past the Earth. ...
... mass less than 3 M, a magnetic field 1012 times stronger than that of the Sun, and a rotation period of roughly 1 second. Pulsars: A pulsar is a source of periodic pulses of radio radiation. These pulses are produced as beams of radio waves from a neutron star’s magnetic poles sweep past the Earth. ...
Explore the Galaxy - Museum of Science, Boston
... Radio Sphere- The boundary of radio transmissions sent from Earth into space, distributed uniformly in a spherical shape with Earth at the center. The earliest signals with enough power to escape the Earth were broadcast in the mid-1930s, and all subsequent signals will continue to extend out into s ...
... Radio Sphere- The boundary of radio transmissions sent from Earth into space, distributed uniformly in a spherical shape with Earth at the center. The earliest signals with enough power to escape the Earth were broadcast in the mid-1930s, and all subsequent signals will continue to extend out into s ...
PowerPoint file - Adin Community Bible Church
... The popular theory is that stars form from vast clouds of gas and dust through gravitational contraction. ...
... The popular theory is that stars form from vast clouds of gas and dust through gravitational contraction. ...
Hertzsprung2 - courses.psu.edu
... A final word about the stars in the night sky: * Majority of stars in the galaxy are low-luminosity cool stars (“red dwarfs”) ...
... A final word about the stars in the night sky: * Majority of stars in the galaxy are low-luminosity cool stars (“red dwarfs”) ...
AST301.Ch18.InterstelMed - University of Texas Astronomy
... same composition as the sun and other stars (i.e. mostly H, some He, and ~1% heavier elements, consistent with stars forming from this gas), except that some elements are depleted , i.e. their abundances are low compared to stars. This is almost certainly because these elements have converted into t ...
... same composition as the sun and other stars (i.e. mostly H, some He, and ~1% heavier elements, consistent with stars forming from this gas), except that some elements are depleted , i.e. their abundances are low compared to stars. This is almost certainly because these elements have converted into t ...
Galactic Address/Stars/Constellations
... • Milky Way Galaxy • Local Group • Virgo Supercluster • Universe ...
... • Milky Way Galaxy • Local Group • Virgo Supercluster • Universe ...
Brichler-powerpoint
... H-R diagram that includes more than 90% of all stars. • These stars are in the middle of their lives. • Our sun is a main sequence star. ...
... H-R diagram that includes more than 90% of all stars. • These stars are in the middle of their lives. • Our sun is a main sequence star. ...
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.