Topic E: Astrophysics E1 Introduction to the Universe.
... elliptical galaxy. if the gas has time to _________________ into a disk before it is all used up, then you get a spiral galaxy. Or perhaps some of the elliptical galaxies are made from merging of other types of galaxies. Observations of distant galaxies indicates that spiral galaxies were more ...
... elliptical galaxy. if the gas has time to _________________ into a disk before it is all used up, then you get a spiral galaxy. Or perhaps some of the elliptical galaxies are made from merging of other types of galaxies. Observations of distant galaxies indicates that spiral galaxies were more ...
stars & galaxies
... The milKy Way… our home iN The sTars… • The Milky Way has a diameter of about 100,000 light years. • The nucleus is 2000 light years thick. • Our sun is located 30,000 light years from the nucleus. • It takes the sun 200 million years to ...
... The milKy Way… our home iN The sTars… • The Milky Way has a diameter of about 100,000 light years. • The nucleus is 2000 light years thick. • Our sun is located 30,000 light years from the nucleus. • It takes the sun 200 million years to ...
The Modern Origins Story: From the Big Bang to Habitable Planets
... Simulation of Collapse of Gas Cloud to Form Stars (Matthew Bate) ...
... Simulation of Collapse of Gas Cloud to Form Stars (Matthew Bate) ...
File - Mr. LaFranca`s Earth Science Class
... Nebula: is a huge, diffuse cloud of gas and dust in space Planet: A celestial body moving in an elliptical orbit around a star. Comet: A small, frozen mass of dust and gas revolving around the sun. Moon: small rocky bodies that orbit a planet Asteroid: small rocky objects that do not orbit a planet ...
... Nebula: is a huge, diffuse cloud of gas and dust in space Planet: A celestial body moving in an elliptical orbit around a star. Comet: A small, frozen mass of dust and gas revolving around the sun. Moon: small rocky bodies that orbit a planet Asteroid: small rocky objects that do not orbit a planet ...
La teoria del big bang y la formacion del Universo
... • Within a few hundred million years after the Big Bang, the hydrogen and helium had pulled together under the force of gravity to form stars, which shine because hydrogen atoms are fusing together to make helium atoms, releasing radiation energy in the process. • When the hydrogen runs out, the s ...
... • Within a few hundred million years after the Big Bang, the hydrogen and helium had pulled together under the force of gravity to form stars, which shine because hydrogen atoms are fusing together to make helium atoms, releasing radiation energy in the process. • When the hydrogen runs out, the s ...
1. What is the HR diagram? 1a. The HR diagram is a plot of a star`s
... On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen burning shell? If not, why not? No because Helium burning requires a ...
... On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen burning shell? If not, why not? No because Helium burning requires a ...
Turbulent Flow-Driven Molecular Cloud Formation: A Solution to the
... by our MHD numerical simulations, in which large-scale H I streams collide to produce dense filamentary structures. This rapid evolution is possible because the H I flows producing and disrupting the cloud have much higher velocities (5-10 km s−1 ) than present in the molecular gas resulting from th ...
... by our MHD numerical simulations, in which large-scale H I streams collide to produce dense filamentary structures. This rapid evolution is possible because the H I flows producing and disrupting the cloud have much higher velocities (5-10 km s−1 ) than present in the molecular gas resulting from th ...
WEEK 8: CSI UCSC: ASTRO EDITION SOLUTIONS This week you
... as a result the core starts to contract. As the core contracts, the density and the temperature increase. Once it gets dense and hot enough, heavier elements can start to fuse (ex. the Sun can now fuse helium into carbon/oxygen), which means the star has found a new source of energy and thermal pres ...
... as a result the core starts to contract. As the core contracts, the density and the temperature increase. Once it gets dense and hot enough, heavier elements can start to fuse (ex. the Sun can now fuse helium into carbon/oxygen), which means the star has found a new source of energy and thermal pres ...
Universe 8e Lecture Chapter 17 Nature of Stars
... The “intrinsic brightness” or luminosity (L) of a star can be determined from a measurement of the star’s apparent brightness (b) and a knowledge of the star’s distance. The surface temperature (T) of a star can be determined from a measurement of the star’s color ...
... The “intrinsic brightness” or luminosity (L) of a star can be determined from a measurement of the star’s apparent brightness (b) and a knowledge of the star’s distance. The surface temperature (T) of a star can be determined from a measurement of the star’s color ...
Placing Our Solar System in Context
... rare among sun-like stars in the Milky Way galaxy? Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to procee ...
... rare among sun-like stars in the Milky Way galaxy? Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to procee ...
LANL Cosmology Summer School Lectures, July 2010
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
Document
... The iron core mass is a (nucleosynthetic) lower limit to the baryonic mass of the neutron star. A large entropy jump characterizes the base of the oxygen shell and may provide a natural location for the mass cut. Naively the baryonic mass of the remnant may be between these two – but this is very cr ...
... The iron core mass is a (nucleosynthetic) lower limit to the baryonic mass of the neutron star. A large entropy jump characterizes the base of the oxygen shell and may provide a natural location for the mass cut. Naively the baryonic mass of the remnant may be between these two – but this is very cr ...
AY2 - Overview of the Universe
... light-years away. She traveled at an average speed very close to the speed of lightsay, 0.9999c. 30) Which of the following best describes the situation according to Jackie? A) She says that the 25-light-year trip takes only a few months and therefore concludes that she is traveling faster than the ...
... light-years away. She traveled at an average speed very close to the speed of lightsay, 0.9999c. 30) Which of the following best describes the situation according to Jackie? A) She says that the 25-light-year trip takes only a few months and therefore concludes that she is traveling faster than the ...
Cloud Formation, Evolution and Destruction
... dilemma is to decide what occurred first: the production of the cloud or the molecules? We all agree that a star-forming cloud must become gravitationally bound. Here, we shall investigate what this implies and what bound states are possible. To do this, we need to bring in concepts from hydrostatic ...
... dilemma is to decide what occurred first: the production of the cloud or the molecules? We all agree that a star-forming cloud must become gravitationally bound. Here, we shall investigate what this implies and what bound states are possible. To do this, we need to bring in concepts from hydrostatic ...
Islip Invitational 2013 Astronomy Examination Student
... e. All of the above are correct. 23. Astronomers studying regions like the Orion Giant Molecular Cloud have observed that a wave of star formation can move through them over many millions of years. What sustains such a wave of star formation in a giant molecular cloud? a. Radio waves from complex mo ...
... e. All of the above are correct. 23. Astronomers studying regions like the Orion Giant Molecular Cloud have observed that a wave of star formation can move through them over many millions of years. What sustains such a wave of star formation in a giant molecular cloud? a. Radio waves from complex mo ...
Our Galaxy -- The Milky Way PowerPoint
... The Sun’s Location in Our Galaxy • William Herschel’s observations – The Solar System is disk-shaped • Faint stars cluster in a band extending in all directions ...
... The Sun’s Location in Our Galaxy • William Herschel’s observations – The Solar System is disk-shaped • Faint stars cluster in a band extending in all directions ...
Global star formation in the Milky Way from the VIALACTEA
... With almost 900 hours observing time is the largest OPEN TIME Herschel KP ...
... With almost 900 hours observing time is the largest OPEN TIME Herschel KP ...
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.