Astronomy 100, Fall 2006 Name: Due: December 5, 2006 at 11 a.m.
... Two models for how stars orbit a galactic center: the “record” model, in which the stars all revolve at the same angular rate around the center, like they were stuck on a record on a turntable, and the “swirling taffy” model, in which stars at a certain distance from the center all move at the same ...
... Two models for how stars orbit a galactic center: the “record” model, in which the stars all revolve at the same angular rate around the center, like they were stuck on a record on a turntable, and the “swirling taffy” model, in which stars at a certain distance from the center all move at the same ...
Stars Notes
... • If any of the core remains it either becomes a neutron star or a black hole. – A black hole is matter that is so compressed that nothing can escape its gravity pull. ...
... • If any of the core remains it either becomes a neutron star or a black hole. – A black hole is matter that is so compressed that nothing can escape its gravity pull. ...
Supernova worksheet with solutions ()
... remain stable for long periods of time, and then expel gas back into space, where it can later form new stars. Below are four stages in the life of a massive star. Describe what happens in each stage, and how energy is generated and used up. Initial formation from a cloud of gas Description: Once a ...
... remain stable for long periods of time, and then expel gas back into space, where it can later form new stars. Below are four stages in the life of a massive star. Describe what happens in each stage, and how energy is generated and used up. Initial formation from a cloud of gas Description: Once a ...
chapter16StarBirth
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure ...
... for infrared and radio photons to escape • Thermal energy then begins to build up inside, increasing the internal pressure ...
The Solar System
... – supernova remnants, expanding at 10,000 km/s – may trigger future star formation? – Neutron stars: mass star but just 10 km across. • Teaspoon weighs 100 million tons! • Seen as Pulsars, flashing beacons in space. ...
... – supernova remnants, expanding at 10,000 km/s – may trigger future star formation? – Neutron stars: mass star but just 10 km across. • Teaspoon weighs 100 million tons! • Seen as Pulsars, flashing beacons in space. ...
Star Cycle Notes
... larger atoms and eventually the star explodes, shedding most of its mass. Red giants expel their mass into space, which eventually condenses and form planetary nebulas. Planetary nebulas, as their name suggests, further condense and form planets. Supergiants explode so violently, they form supernova ...
... larger atoms and eventually the star explodes, shedding most of its mass. Red giants expel their mass into space, which eventually condenses and form planetary nebulas. Planetary nebulas, as their name suggests, further condense and form planets. Supergiants explode so violently, they form supernova ...
Chapter 11
... Triggering Star Formation (1) Previous star formation can trigger further star formation through: a) Shocks from ...
... Triggering Star Formation (1) Previous star formation can trigger further star formation through: a) Shocks from ...
Star Formation: Interstellar Gas and Dust
... • Blows away gas trying to fall onto forming star. ...
... • Blows away gas trying to fall onto forming star. ...
The Evolution of Stars - hrsbstaff.ednet.ns.ca
... the natural phenomenon by which all objects with mass attract other objects. Without gravity the universe would be a very different place. ...
... the natural phenomenon by which all objects with mass attract other objects. Without gravity the universe would be a very different place. ...
REVIEW: STAR`S TEST
... Explain how the e and m are related. A small amount of _____________ can become a huge amount of ____________ What is the speed of light ? List the visible light from longest to shortest wavelengths. ...
... Explain how the e and m are related. A small amount of _____________ can become a huge amount of ____________ What is the speed of light ? List the visible light from longest to shortest wavelengths. ...
THE LIFE CYCLE OF A STAR
... A protostar is a large mass that forms by contraction out of the gas of a giant molecular cloud in the interstellar medium. The protostellar phase is an early stage in the process of star formation. For a one solar-mass star it lasts about 100,000 years. It starts with a core of increased density in ...
... A protostar is a large mass that forms by contraction out of the gas of a giant molecular cloud in the interstellar medium. The protostellar phase is an early stage in the process of star formation. For a one solar-mass star it lasts about 100,000 years. It starts with a core of increased density in ...
Properties of Stars
... Measuring Distance to Stars • Parallax is determined by taking a picture of a star at one time, and another picture six months later; using the angle between its apparent shift, astronomers can determine how far away it is • The nearest stars have large parallax angles, while those of distant stars ...
... Measuring Distance to Stars • Parallax is determined by taking a picture of a star at one time, and another picture six months later; using the angle between its apparent shift, astronomers can determine how far away it is • The nearest stars have large parallax angles, while those of distant stars ...
Star Life Guided Notes
... determines the fate of a star. gravityand _____ fusion The two forces acting on a star are ____ When a star reaches the end of its life it begins to helium and it ______. fuse ______ swells planetary When fusion stops a typical star will producenebula a __ white dwarf and become a ______ _____. Even ...
... determines the fate of a star. gravityand _____ fusion The two forces acting on a star are ____ When a star reaches the end of its life it begins to helium and it ______. fuse ______ swells planetary When fusion stops a typical star will producenebula a __ white dwarf and become a ______ _____. Even ...
30-2 Directed Reading
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
Star project
... supernova. Clumps begin to form in the cloud, and compress and heat up. Eventually, a protostar is formed, which is the core of the star. • The protostar heats up so much and collects so much dust and gas that it releases a massive amount of gas in the form of a jet, called a bipolar. The dust event ...
... supernova. Clumps begin to form in the cloud, and compress and heat up. Eventually, a protostar is formed, which is the core of the star. • The protostar heats up so much and collects so much dust and gas that it releases a massive amount of gas in the form of a jet, called a bipolar. The dust event ...
The HR Diagram
... • Where are stars most of their lives? • Where are they when they begin to die? • What are they after they use up their ...
... • Where are stars most of their lives? • Where are they when they begin to die? • What are they after they use up their ...
Introduction to Astrophysics Tutorial 4: Supernovae
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
Homework, August 29, 2002 AST110-6
... 1. If nuclear fusion of hydrogen in the core of the Sun were to stop now, what would we see on the surface of the Sun tomorrow? Why? Will we be able to tell that hydrogen burning in the core has stopped? How? (20pt) (Hint: What particles that are generated by the fusion of hydrogen can escape from t ...
... 1. If nuclear fusion of hydrogen in the core of the Sun were to stop now, what would we see on the surface of the Sun tomorrow? Why? Will we be able to tell that hydrogen burning in the core has stopped? How? (20pt) (Hint: What particles that are generated by the fusion of hydrogen can escape from t ...
MASSACHUSETTS INSTITUTE OF TECHNOLOGY
... symmetry). For the case of hydrostatic equilibrium, r¨ = 0. (Note that for a collapsing cloud, the mass enclosed by the collapsing surface remains constant as the density increases.) Consider the collapse of a uniform-density giant molecular cloud with temperature T = 150 K and number density 108 cm ...
... symmetry). For the case of hydrostatic equilibrium, r¨ = 0. (Note that for a collapsing cloud, the mass enclosed by the collapsing surface remains constant as the density increases.) Consider the collapse of a uniform-density giant molecular cloud with temperature T = 150 K and number density 108 cm ...
Masers and high mass star formation Claire Chandler
... • Ionization phenomena associated with massive SF: UCHII regions • Different environments observed has led to the suggestion that different mechanisms (or modes) apply to low- and high-mass SF ...
... • Ionization phenomena associated with massive SF: UCHII regions • Different environments observed has led to the suggestion that different mechanisms (or modes) apply to low- and high-mass SF ...
Lab 21.1 Classifying Stars
... 1. Compare the star’s mass to its luminosity and to its temperature. Can you find any basic relationship between these traits? (i.e. the greater the mass, the ….) _____________________ ______________________________________________________________________________ 2. (a) What is a red giant? ________ ...
... 1. Compare the star’s mass to its luminosity and to its temperature. Can you find any basic relationship between these traits? (i.e. the greater the mass, the ….) _____________________ ______________________________________________________________________________ 2. (a) What is a red giant? ________ ...
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.