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... • High mass-loss rates, and cool effective temperatures (~3000 K) • A dust shell hides most of the stellar luminosity and so the stars are seen only in the infrared. ...
... • High mass-loss rates, and cool effective temperatures (~3000 K) • A dust shell hides most of the stellar luminosity and so the stars are seen only in the infrared. ...
Initial Evolution-The Main Sequence
... Two scenarios: stars with as mass less than 8 times the mass of the sun and stars with a mass greater than 8 times the mass of the sun. ...
... Two scenarios: stars with as mass less than 8 times the mass of the sun and stars with a mass greater than 8 times the mass of the sun. ...
Homework 1
... All stars start off as a cloud of dust. Over time the dust starts to clump together and form what is called a protostar. As the protostar becomes more massive the gravitational pressure on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the t ...
... All stars start off as a cloud of dust. Over time the dust starts to clump together and form what is called a protostar. As the protostar becomes more massive the gravitational pressure on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the t ...
The H-R Diagram
... • - once in a great while a neutrino will hit an electron and deposit its energy, accelerating the electron to almost the (vacuum) speed of light. This rapid acceleration causes the electron to give of photons of light = Cerenkov radiation. • Cerenkov radiation is given off when a charge moves faste ...
... • - once in a great while a neutrino will hit an electron and deposit its energy, accelerating the electron to almost the (vacuum) speed of light. This rapid acceleration causes the electron to give of photons of light = Cerenkov radiation. • Cerenkov radiation is given off when a charge moves faste ...
Space Science Review Vocabulary: Nebula Proto Star Main
... Absolute Magnitude Apparent Magnitude ...
... Absolute Magnitude Apparent Magnitude ...
Astronomy Exam #2 for the 10
... Giant molecular clouds are very large clouds of gas and dust in the inter-stellar medium. These clouds are composed mostly of H2 and He with trace amounts of other gases and microscopic pieces of rock and ices that astronomers collectively call dust. These GMC’s can be 300 ly in diameter and have ma ...
... Giant molecular clouds are very large clouds of gas and dust in the inter-stellar medium. These clouds are composed mostly of H2 and He with trace amounts of other gases and microscopic pieces of rock and ices that astronomers collectively call dust. These GMC’s can be 300 ly in diameter and have ma ...
Origin of the Solar System
... •contains the heavier elements (Fe, Si, O) •rocky shell over a metallic core •Accretion began 4.567 billion years ago •It took about 0.1 billion years (100 million years) for planets to form ...
... •contains the heavier elements (Fe, Si, O) •rocky shell over a metallic core •Accretion began 4.567 billion years ago •It took about 0.1 billion years (100 million years) for planets to form ...
Astronomy 110 Announcements: 11.1 Properties of Stars
... Spectral types are further broken down to sub-classes by numbers from 0 to 9 (hotter to cooler) Lines in a star’s spectrum correspond to a spectral type that reveals its temperature (Hottest) ...
... Spectral types are further broken down to sub-classes by numbers from 0 to 9 (hotter to cooler) Lines in a star’s spectrum correspond to a spectral type that reveals its temperature (Hottest) ...
HR Diagram Lab Handout
... Background: You are about to create your own HR Diagram, a chart that revolutionized the study of stars. You will have a labeled chart and a series of points to plot. From these points, you can deduce a lot of information about stars! Please read the directions in each step of the activity closely b ...
... Background: You are about to create your own HR Diagram, a chart that revolutionized the study of stars. You will have a labeled chart and a series of points to plot. From these points, you can deduce a lot of information about stars! Please read the directions in each step of the activity closely b ...
lec03_30sep2011
... -~7% of solar-type stars have >Mj planets in the “terrestrial planet” region. Extrapolation of current incompeteness suggests >12% w/planets @ <20 AU. - multiple planetary systems are ~common - planetary resonances are ~common What can explain these properties? ...
... -~7% of solar-type stars have >Mj planets in the “terrestrial planet” region. Extrapolation of current incompeteness suggests >12% w/planets @ <20 AU. - multiple planetary systems are ~common - planetary resonances are ~common What can explain these properties? ...
HR Diagrams
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
... Do you think that taller students tend to weigh more or less than shorter students? You could examine this by plotting the students in your class on a graph, with height on one axis and weight on the other. Each student would be plotted as a point on the graph. What do you think that graph would loo ...
PHYS 390 Lecture 29 - White dwarfs and neutron stars 29
... Sirius was observed (by a new 18-inch refractor) to be a binary system in 1862, almost 20 years after it was proposed to be such as system by Friedrich Bessel. The smaller of the binary pair has a mass now quoted at 1.05±0.03 solar masses, and a surface temperature (determined half a century later) ...
... Sirius was observed (by a new 18-inch refractor) to be a binary system in 1862, almost 20 years after it was proposed to be such as system by Friedrich Bessel. The smaller of the binary pair has a mass now quoted at 1.05±0.03 solar masses, and a surface temperature (determined half a century later) ...
Astro 10: Introductory Astronomy
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
SSS in young stellar populations: progenitors of the
... • SSS in these systems could be TNR on white dwarf once it accretes critical mass from Be disk • WDs could experience accretion and outburst cycles like in novae, and possible gain in mass with time • WDs initially massive, so require less mass to reach MCh • Mass accretion can be more efficient if ...
... • SSS in these systems could be TNR on white dwarf once it accretes critical mass from Be disk • WDs could experience accretion and outburst cycles like in novae, and possible gain in mass with time • WDs initially massive, so require less mass to reach MCh • Mass accretion can be more efficient if ...
The Universe and Galaxies - West Jefferson Local Schools
... - time is required for light to travel through space - light travels a little over 8 minutes from the sun to earth - the farther away an object/star is, the longer it takes for light to get to us, and the older the light is when it gets to us = “Light is OLD” - we see the past of other stars in the ...
... - time is required for light to travel through space - light travels a little over 8 minutes from the sun to earth - the farther away an object/star is, the longer it takes for light to get to us, and the older the light is when it gets to us = “Light is OLD” - we see the past of other stars in the ...
Sun - TeacherWeb
... Each element makes a unique emission spectrum Spectral lines tell us which elements are in a star. Continuous Spectrum ...
... Each element makes a unique emission spectrum Spectral lines tell us which elements are in a star. Continuous Spectrum ...
STUDY GUIDE FOR CHAPTER 1
... 4. You always know the brightness if you can see the star so this allows you to determine the distance to the star. 5. This works for any star that we can see well enough to get an accurate spectrum. This includes stars in our galaxy that are too far away to use parallax. ...
... 4. You always know the brightness if you can see the star so this allows you to determine the distance to the star. 5. This works for any star that we can see well enough to get an accurate spectrum. This includes stars in our galaxy that are too far away to use parallax. ...
Solar System Formation
... History of SS Formation theories 2 Theories of type (ii): • A passing star pulled some of the Sun’s atmosphere off via tidal forces. This former atmospheric material then coalesced and formed the planets (early 1900s) • The Sun captured material from passing interstellar clouds (1940s) ...
... History of SS Formation theories 2 Theories of type (ii): • A passing star pulled some of the Sun’s atmosphere off via tidal forces. This former atmospheric material then coalesced and formed the planets (early 1900s) • The Sun captured material from passing interstellar clouds (1940s) ...
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.