Astronomy Test Objective 1: Origins of the Universe Multiple Choice
... 8. Small, massive dense object that has a gravity so immense that nothing – not even light – can escape it. Short Answer ...
... 8. Small, massive dense object that has a gravity so immense that nothing – not even light – can escape it. Short Answer ...
The Nuclear Reactions
... in the CNO Cycle requires a Carbon nucleus (6 p+) to react with a proton it requires higher temperatures and is much more temperature sensitive than the P-P Chain (The energy produced is proportional to T20 for the CNO cycle vs T4 for the P-P Chain). Stars of mass greater than about 1.2 M with core ...
... in the CNO Cycle requires a Carbon nucleus (6 p+) to react with a proton it requires higher temperatures and is much more temperature sensitive than the P-P Chain (The energy produced is proportional to T20 for the CNO cycle vs T4 for the P-P Chain). Stars of mass greater than about 1.2 M with core ...
Black Hole at Galactic Center
... Mystery at the Galactic Core Here is a simulation plot* of 21 stellar motions around the core of our Milky Way Galaxy. Notice that in the 16 years we have been following these stars, S0-2 has managed to finish one complete orbit around the mysterious, non-luminous object at the galactic core. S0-2 i ...
... Mystery at the Galactic Core Here is a simulation plot* of 21 stellar motions around the core of our Milky Way Galaxy. Notice that in the 16 years we have been following these stars, S0-2 has managed to finish one complete orbit around the mysterious, non-luminous object at the galactic core. S0-2 i ...
PART II: Life of a Star
... composition → complex history of Galaxy. This revelation spawned numerous branches of Astrophysics. • Metal-poor stars in particular can provide constraints on: • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be ...
... composition → complex history of Galaxy. This revelation spawned numerous branches of Astrophysics. • Metal-poor stars in particular can provide constraints on: • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be ...
Lecture5
... happens. The intensity (brightness) of the binary vs time curve is called `light curve’. Then the shape of the light curve can often determine various useful parameters, e.g., the inclination angle , nature of the stellar atmosphere, and sometimes even stellar radius. See class notes and Fig. II-36 ...
... happens. The intensity (brightness) of the binary vs time curve is called `light curve’. Then the shape of the light curve can often determine various useful parameters, e.g., the inclination angle , nature of the stellar atmosphere, and sometimes even stellar radius. See class notes and Fig. II-36 ...
Stellar Forces
... electrons) is very inefficient as electrons collide often with other particles. However, ...
... electrons) is very inefficient as electrons collide often with other particles. However, ...
Goal: To understand the HR diagram
... • If we plotted all the stars from a single cluster what might we get? • First we should ask 2 questions: • 1) How do the distances from us compare to all the stars in the cluster (close to same, or not close)? • 2) How do the ages of the stars in the cluster compare? ...
... • If we plotted all the stars from a single cluster what might we get? • First we should ask 2 questions: • 1) How do the distances from us compare to all the stars in the cluster (close to same, or not close)? • 2) How do the ages of the stars in the cluster compare? ...
Chapter 3 - BITS Pilani
... center of the Sun using the Gas pressure term alone and using the value for pressure we derived in the previous example. ...
... center of the Sun using the Gas pressure term alone and using the value for pressure we derived in the previous example. ...
Hot Stars With Cool Companions
... The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevant physics involved during and after the formation of the secondary. The dominant mode of binary star formation is thought to be molecular core fragmentation (Boss & Bodenheimer 1979; Bo ...
... The multiplicity of A- and B-type stars can also help constrain the binary star formation mechanism and the relevant physics involved during and after the formation of the secondary. The dominant mode of binary star formation is thought to be molecular core fragmentation (Boss & Bodenheimer 1979; Bo ...
WIMPs vs. MACHOS: What's the Matter?
... million stars This significantly exceeds the single event expected from “known” stars in the Galaxy ...
... million stars This significantly exceeds the single event expected from “known” stars in the Galaxy ...
Compact Extragalactic Star Formation
... • What are the properties of the youngest massive star clusters? How do they evolve to become globular clusters today? What is the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How ...
... • What are the properties of the youngest massive star clusters? How do they evolve to become globular clusters today? What is the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How ...
9.1 Introduction 9.2 Static Models
... by replacing the differential equations with difference equations and approximating the internal structure of a star by a series of concentric shells separated by a small, but finite, radial distance δr. For example, if the pressure in shell i is Pi , the pressure in the next shell is Pi+1 = Pi +(∆P ...
... by replacing the differential equations with difference equations and approximating the internal structure of a star by a series of concentric shells separated by a small, but finite, radial distance δr. For example, if the pressure in shell i is Pi , the pressure in the next shell is Pi+1 = Pi +(∆P ...
1 - Università degli Studi dell`Insubria
... >H in the hard stage is proportional to a -/2 >K is typically positive, but the eccentricity evoution of the binary is modest >MBHB-star interactions flatten the stellar distribution >Interacting stars typically corotate with the MBHB >A mass of the order of 0.7M is ejected from the bulge on nearly ...
... >H in the hard stage is proportional to a -/2 >K is typically positive, but the eccentricity evoution of the binary is modest >MBHB-star interactions flatten the stellar distribution >Interacting stars typically corotate with the MBHB >A mass of the order of 0.7M is ejected from the bulge on nearly ...
Basics about stars
... There are different types of variables appearing in the HRD. Basically, whenever the ”instability strip” overlaps with an actual stellar population variable stars are found. • δ-Cepheids : Luminosities range from 300−3000L and periods between 1-50 days. Brightness variation during 1 period can be u ...
... There are different types of variables appearing in the HRD. Basically, whenever the ”instability strip” overlaps with an actual stellar population variable stars are found. • δ-Cepheids : Luminosities range from 300−3000L and periods between 1-50 days. Brightness variation during 1 period can be u ...
1 - Stars: Introduction
... with a distribu)on of energy over the wavelengths that depends on temperature T Blackbody radiaEon: photons are in equilibrium with the system à Stefan-Boltzmann law: ...
... with a distribu)on of energy over the wavelengths that depends on temperature T Blackbody radiaEon: photons are in equilibrium with the system à Stefan-Boltzmann law: ...
Evolved massive stars in W33 and in GMC G23.3-0.3
... Abstract. We conducted infrared spectroscopic observations of bright stars in the direction of the molecular clouds W33 and GMC G23.3−0.3. We compared stellar spectro-photometric distances with parallactic distances to these regions, and we were able to assess the association of the detected massive ...
... Abstract. We conducted infrared spectroscopic observations of bright stars in the direction of the molecular clouds W33 and GMC G23.3−0.3. We compared stellar spectro-photometric distances with parallactic distances to these regions, and we were able to assess the association of the detected massive ...
Topic/Objective: ______ _____ Full Name: __________ Class: __
... Betelguese is about one ten-millionth of our Sun One star is so dense that one teaspoon would weight more than a ton on Earth Temperature of stars vary Stars have different colors which indicate different temperatures Cool stars are red in color Mid-temp are yellower in color Hot stars ...
... Betelguese is about one ten-millionth of our Sun One star is so dense that one teaspoon would weight more than a ton on Earth Temperature of stars vary Stars have different colors which indicate different temperatures Cool stars are red in color Mid-temp are yellower in color Hot stars ...
Chapter12 (with interactive links)
... in the expanding outer layers, causing the planetary nebula that we can observe. Planetary nebulae do not last forever – eventually the gas disperses. ...
... in the expanding outer layers, causing the planetary nebula that we can observe. Planetary nebulae do not last forever – eventually the gas disperses. ...
THE SUN - Halton District School Board
... In the core, the sun’s large gravitation force compresses hydrogen atoms together and fuses their nuclei creating helium atoms. Each second the Sun converts about 600,000,000 tons of hydrogen nuclei into helium nuclei. The fusion reaction creates an explosion in the core that causes massive amounts ...
... In the core, the sun’s large gravitation force compresses hydrogen atoms together and fuses their nuclei creating helium atoms. Each second the Sun converts about 600,000,000 tons of hydrogen nuclei into helium nuclei. The fusion reaction creates an explosion in the core that causes massive amounts ...
supplemental materials.
... Color-Magnitude Diagrams (CMDs) are plots that compare the magnitudes (luminosities) of stars in different wavelengths of light (colors). High non-linear correlations among the mass, color and surface temperature of newly formed stars induce a long narrow curved point cloud in a CMD known as the mai ...
... Color-Magnitude Diagrams (CMDs) are plots that compare the magnitudes (luminosities) of stars in different wavelengths of light (colors). High non-linear correlations among the mass, color and surface temperature of newly formed stars induce a long narrow curved point cloud in a CMD known as the mai ...
Homework 1
... on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the temperature to increase. Seeing as the mass of the protostar is larger it can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and tempera ...
... on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the temperature to increase. Seeing as the mass of the protostar is larger it can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and tempera ...
Earth Science 25.2B : Stellar Evolution
... from a white dwarf would weigh several tons. Densities this great are possible only when electrons are displaced inward from their regular orbits, around an atom’s nucleus, allowing the atoms to take up less than the “normal” amount of space. ...
... from a white dwarf would weigh several tons. Densities this great are possible only when electrons are displaced inward from their regular orbits, around an atom’s nucleus, allowing the atoms to take up less than the “normal” amount of space. ...
PowerPoint - Chandra X
... in the Cassiopeia A supernova remnant over the past ten years have revealed a 4% decline in the neutron star’s surface temperature, which is ~2 MK. ...
... in the Cassiopeia A supernova remnant over the past ten years have revealed a 4% decline in the neutron star’s surface temperature, which is ~2 MK. ...
Constellations & Stars - Toms River Regional Schools :: Home
... 2. Taurus (the Bull) • Follow the line made by Orion’s belt up & to the right • Aldebaran- Red star that is the eye of the bull is the 13th brightest in the ...
... 2. Taurus (the Bull) • Follow the line made by Orion’s belt up & to the right • Aldebaran- Red star that is the eye of the bull is the 13th brightest in the ...
E.S. 14: The Universe Universe Formation: The Big Bang Theory
... B. Spiral galaxies have spiral arms that start close to the center. i. Ex: The Milky Way ...
... B. Spiral galaxies have spiral arms that start close to the center. i. Ex: The Milky Way ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.