Lecture course problems
... 43 000 km h1. Calculate the Doppler shifts for the H line observed from points on the extreme left and extreme right of Jupiter’s equator, as viewed from earth. What would be the Doppler shift for a point observed in the centre of the planet as viewed ...
... 43 000 km h1. Calculate the Doppler shifts for the H line observed from points on the extreme left and extreme right of Jupiter’s equator, as viewed from earth. What would be the Doppler shift for a point observed in the centre of the planet as viewed ...
printer-friendly sample test questions
... A. The once-smaller universe is expanding in all directions. B. The Sun and Earth are located at the center of the universe. C. Everything in the universe is moving the same direction. D. Massive black holes are drawing galaxies away from Earth. 4. We know that nearly all galaxies are moving away fr ...
... A. The once-smaller universe is expanding in all directions. B. The Sun and Earth are located at the center of the universe. C. Everything in the universe is moving the same direction. D. Massive black holes are drawing galaxies away from Earth. 4. We know that nearly all galaxies are moving away fr ...
10.1 The Solar Neighborhood Barnard`s Star
... Nearest star to the Sun: Proxima Centauri, which is a member of a 3-star system: Alpha Centauri complex (3 stars orbiting each other) Model of distances: Sun is a marble, Earth is a grain of sand ...
... Nearest star to the Sun: Proxima Centauri, which is a member of a 3-star system: Alpha Centauri complex (3 stars orbiting each other) Model of distances: Sun is a marble, Earth is a grain of sand ...
STAAR Science Tutorial 35 TEK 8.8B: The Sun
... Sun) is Proxima Centauri, which is about 4.2 light years away from Earth. This is 263,000 times further away from Earth than our Sun. (Our Sun is 0.000016 lightyears away from Earth.) While there are 11 stars within 10 light-years of Earth, most of the other stars visible in the night sky are many t ...
... Sun) is Proxima Centauri, which is about 4.2 light years away from Earth. This is 263,000 times further away from Earth than our Sun. (Our Sun is 0.000016 lightyears away from Earth.) While there are 11 stars within 10 light-years of Earth, most of the other stars visible in the night sky are many t ...
Eksamination in FY2450 Astrophysics Wednesday June 8
... The higher the excitation energy of the atomic transition, the higher the temperature where the spectral line appears. For example, it takes less energy to remove the first electron from a helium atom than it takes to excite the second electron afterwards. Therefore the lines of neutral helium appea ...
... The higher the excitation energy of the atomic transition, the higher the temperature where the spectral line appears. For example, it takes less energy to remove the first electron from a helium atom than it takes to excite the second electron afterwards. Therefore the lines of neutral helium appea ...
Lecture 11: The Internal Structure of Stars
... Central Pressure and Temperature in the Sun The observation that the Sun is in hydrostatic equilibrium (along with the mass and radius) gives us enough information to estimate the central pressure and temperature of the Sun. We can use the mass and the radius to estimate how much the force of gravit ...
... Central Pressure and Temperature in the Sun The observation that the Sun is in hydrostatic equilibrium (along with the mass and radius) gives us enough information to estimate the central pressure and temperature of the Sun. We can use the mass and the radius to estimate how much the force of gravit ...
Stars - WhatisOutThere
... helium. These are the two lightest elements. They shine by burning the hydrogen into helium in their cores, then later in life they create heavier elements. Most stars have heavy elements, like carbon, nitrogen, oxygen and iron but only small amounts. These elements came from the stars that existed ...
... helium. These are the two lightest elements. They shine by burning the hydrogen into helium in their cores, then later in life they create heavier elements. Most stars have heavy elements, like carbon, nitrogen, oxygen and iron but only small amounts. These elements came from the stars that existed ...
talk
... -- gas ≥ stars. -- subsolar metallicity outer conditionsof lines from In recent yearsdisk better measurements HII regions have shown that electron temps rise with distance, resulting in weaker gradients. -- slowly varying gravitational potential ==> low tidal forces on clouds -- low large-scale ma ...
... -- gas ≥ stars. -- subsolar metallicity outer conditionsof lines from In recent yearsdisk better measurements HII regions have shown that electron temps rise with distance, resulting in weaker gradients. -- slowly varying gravitational potential ==> low tidal forces on clouds -- low large-scale ma ...
Last time: looked at proton-proton chain to convert Hydrogen into
... Young stars which are still accreting material are called T-Tauri Stars. Because mass is piling on, they sometimes have explosive outbursts. ...
... Young stars which are still accreting material are called T-Tauri Stars. Because mass is piling on, they sometimes have explosive outbursts. ...
Summary of Cool Stars 13 - JILA - University of Colorado Boulder
... • (7) “Of course we need more candidates and more data.” • (8) “The synthetic models are wrong. They are always wrong.” • (9) “I think that this thing is running out of battery.” • (10) “In order to give you the impression that we have done our job…” • (11) “The next talk will be on the weather in H ...
... • (7) “Of course we need more candidates and more data.” • (8) “The synthetic models are wrong. They are always wrong.” • (9) “I think that this thing is running out of battery.” • (10) “In order to give you the impression that we have done our job…” • (11) “The next talk will be on the weather in H ...
Exam Study Guide
... 98. According to the Chart of Stellar Evolution (see Reference Item 7), planetary nebula can form from main sequence stars of mass … UNIT 8 — Galaxies and Cosmology — Bits of Chapters 15-18 100. What makes Cephied Variables very useful for measuring distances? 101. Contrast the motion of the disk st ...
... 98. According to the Chart of Stellar Evolution (see Reference Item 7), planetary nebula can form from main sequence stars of mass … UNIT 8 — Galaxies and Cosmology — Bits of Chapters 15-18 100. What makes Cephied Variables very useful for measuring distances? 101. Contrast the motion of the disk st ...
File
... resembles an ant when observed using ground-based telescopes. The nebula lies within our galaxy between 3,000 and 6,000 light years from Earth . ...
... resembles an ant when observed using ground-based telescopes. The nebula lies within our galaxy between 3,000 and 6,000 light years from Earth . ...
Charcteristic of Stars Powerpoint C
... times the radius of Earth. So the sun would equal 1 solar radius. • In comparison white dwarfs are about the same size as Earth and would equal 0.01 solar radius. Supergiants can have sizes up to 1,000 solar radii. ...
... times the radius of Earth. So the sun would equal 1 solar radius. • In comparison white dwarfs are about the same size as Earth and would equal 0.01 solar radius. Supergiants can have sizes up to 1,000 solar radii. ...
Document
... Globular cluster – tight groups of hundreds of thousands of very old stars Open cluster - contain less than a few hundred members, and are often very young - may eventually become disrupted over time and no longer gravitational bound – move in same direction in space – referred to as stellar ass ...
... Globular cluster – tight groups of hundreds of thousands of very old stars Open cluster - contain less than a few hundred members, and are often very young - may eventually become disrupted over time and no longer gravitational bound – move in same direction in space – referred to as stellar ass ...
File
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
File - Awakening in Grade 6
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
... What is the Zodiac? Earth orbits our Sun once each year. Viewed from Earth, our Sun appears to trace a circular path. This path defines a plane called the plane of the ecliptic (or just the ecliptic). The zodiac is the group (or “belt”) of constellations that fall along the plane of the ecliptic. ...
File - Mr. Catt`s Class
... When a red giant reaches the stage where it has a carbon core, – the heat from the shrinking core ignites helium fusion in a shell around it, ...
... When a red giant reaches the stage where it has a carbon core, – the heat from the shrinking core ignites helium fusion in a shell around it, ...
The Hertzsprung-Russell Diagram
... 4. Label these stars as the “main sequence stars.” 5. Circle the group of ten stars above the main sequence. 6. Label these stars as the “red giant stars.” 7. Circle the group of five stars below the main sequence. 8. Label these stars as the “white dwarf stars.” ...
... 4. Label these stars as the “main sequence stars.” 5. Circle the group of ten stars above the main sequence. 6. Label these stars as the “red giant stars.” 7. Circle the group of five stars below the main sequence. 8. Label these stars as the “white dwarf stars.” ...
Answer to question 1 - Northwestern University
... •The result is that the envelope then comes falling down, • Over shoots inward • Then starts over ...
... •The result is that the envelope then comes falling down, • Over shoots inward • Then starts over ...
Characteristics of Stars (Ph)
... Characteristics of Stars Imagine you could travel to the stars at the speed of light. To travel from Earth to the sun would take about 8 minutes, not very long for such a long trip! Yet the next nearest star, Proxima Centauri, is much farther away—a trip to Proxima Centauri would take 4.2 years! ...
... Characteristics of Stars Imagine you could travel to the stars at the speed of light. To travel from Earth to the sun would take about 8 minutes, not very long for such a long trip! Yet the next nearest star, Proxima Centauri, is much farther away—a trip to Proxima Centauri would take 4.2 years! ...
Chapter 13 section 3
... sequence. Scientists also wondered what happened when a star used up its hydrogen fuel. Now, there are theories about how stars evolve, or change over time. These theories also explain what makes stars different from one another, and what happens when a star “dies.” When a star uses up its hydrogen, ...
... sequence. Scientists also wondered what happened when a star used up its hydrogen fuel. Now, there are theories about how stars evolve, or change over time. These theories also explain what makes stars different from one another, and what happens when a star “dies.” When a star uses up its hydrogen, ...
Evolution of a Protostar
... A life track illustrates a star's surface temperature and luminosity at different moments in time. ...
... A life track illustrates a star's surface temperature and luminosity at different moments in time. ...
Document
... Students will learn how to interpret observational characteristics of stars in terms of the underlying physical parameters You should gain an understanding of how stars of different mass evolve, and what end products are produced Students should learn what causes planetary nebulae and supernovae You ...
... Students will learn how to interpret observational characteristics of stars in terms of the underlying physical parameters You should gain an understanding of how stars of different mass evolve, and what end products are produced Students should learn what causes planetary nebulae and supernovae You ...
Measuring Stars
... •Observe the star – determine it’s brightness B •Measure its spectral type from spectrum •Deduce its luminosity from the HertzsprungRussell Diagram •Find its distance from: L = 4d2B ...
... •Observe the star – determine it’s brightness B •Measure its spectral type from spectrum •Deduce its luminosity from the HertzsprungRussell Diagram •Find its distance from: L = 4d2B ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.