November | Activity of the Month
... We are travelling on the Earth through space. Space, or our universe, is a big place, way bigger than we can really imagine, and it’s busy. Look out on a dark clear night and you’ll see millions of stars, some dying and others being born, and there are billions of galaxies or star cities, some that ...
... We are travelling on the Earth through space. Space, or our universe, is a big place, way bigger than we can really imagine, and it’s busy. Look out on a dark clear night and you’ll see millions of stars, some dying and others being born, and there are billions of galaxies or star cities, some that ...
The Milky Way
... I. Making Stars from the Interstellar Medium A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
... I. Making Stars from the Interstellar Medium A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
The Milky Way - Houston Community College System
... I. Making Stars from the Interstellar Medium A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
... I. Making Stars from the Interstellar Medium A. Star Birth in Giant Molecular Clouds B. Heating By Contraction C. Protostars II. The Orion Nebula: Evidence of Star Formation A. Observing Star Formation B. Contagious Star Formation III. Young Stellar Objects and Protostellar Disks ...
Goal: To understand how stars form.
... It doesn’t stop there • When you form stars you don’t form them one system at a time. • The starting Giant Molecular Cloud is often 10 to 100 light years across. • The mass of these clouds are tens of thousands of times more than the mass of our sun. • So…. ...
... It doesn’t stop there • When you form stars you don’t form them one system at a time. • The starting Giant Molecular Cloud is often 10 to 100 light years across. • The mass of these clouds are tens of thousands of times more than the mass of our sun. • So…. ...
STAR LIGHT, STAR BRIGHT
... 5. What does the color of a star indicate about the star? ___________________________________ 6. Identify the temperature associated with each color, and include an example of a star that would appear each color. Temperature Example Red: ___________________________________ ...
... 5. What does the color of a star indicate about the star? ___________________________________ 6. Identify the temperature associated with each color, and include an example of a star that would appear each color. Temperature Example Red: ___________________________________ ...
The Triple-Ring Nebula: Fingerprint of a Binary Merger
... was very unusual; most importantly, the outer layers of the star had an abundance of helium (as a fraction of the total composition) that was about a factor of 2 larger than the expected abundance, as if part of the material from the core, where helium has been produced during the previous evolution ...
... was very unusual; most importantly, the outer layers of the star had an abundance of helium (as a fraction of the total composition) that was about a factor of 2 larger than the expected abundance, as if part of the material from the core, where helium has been produced during the previous evolution ...
Exploring the Habitable Zone for Kepler planetary candidates
... planetary candidates [1]. We use atmospheric models to explore the potential for habitability of Kepler planetary candidates. We focus on the circumstellar HZ, that was defined by Kasting et al. [3] as an annulus around a star where a planet with an atmosphere and a sufficiently large water content ...
... planetary candidates [1]. We use atmospheric models to explore the potential for habitability of Kepler planetary candidates. We focus on the circumstellar HZ, that was defined by Kasting et al. [3] as an annulus around a star where a planet with an atmosphere and a sufficiently large water content ...
Integrative Studies 410 Our Place in the Universe
... thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
... thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
Dead Stars - University of Iowa Astrophysics
... Sirius B (1.02 versus 2.40 solar masses for Sirius A) • Even though it is hotter than Sirius A, it is much fainter (look at difference in absolute magnitudes • The only way to do this is with small WD radius ...
... Sirius B (1.02 versus 2.40 solar masses for Sirius A) • Even though it is hotter than Sirius A, it is much fainter (look at difference in absolute magnitudes • The only way to do this is with small WD radius ...
Dead Stars They do exist! The white dwarf stars
... “Most stars end their lives as white dwarfs. These glowing embers scattered throughout space are a galaxy’s memory of its past glory. Because no fusion occurs in their interiors, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy”…Car ...
... “Most stars end their lives as white dwarfs. These glowing embers scattered throughout space are a galaxy’s memory of its past glory. Because no fusion occurs in their interiors, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy”…Car ...
pg. 271 - Cornell University
... in the absolute flux is 20%–25%. The only exceptions are [Ne vi] (this line is measured at the edge of the spectrum in SL1 and is noisy) and the [Si ii] lines with uncertainties of 50% and 30%, respectively. Absolute flux calibration of the IRS instrument is ongoing, and these uncertainties will dec ...
... in the absolute flux is 20%–25%. The only exceptions are [Ne vi] (this line is measured at the edge of the spectrum in SL1 and is noisy) and the [Si ii] lines with uncertainties of 50% and 30%, respectively. Absolute flux calibration of the IRS instrument is ongoing, and these uncertainties will dec ...
Slide 1
... Electrons being ejected out of an atom. Electrons being lifted into an excited state in an atom. Electrons annihilating on their anti-particles. Two atomic nuclei combining to form a heavier nucleus. A heavy atomic nucleus being split up into two lighter nuclei. ...
... Electrons being ejected out of an atom. Electrons being lifted into an excited state in an atom. Electrons annihilating on their anti-particles. Two atomic nuclei combining to form a heavier nucleus. A heavy atomic nucleus being split up into two lighter nuclei. ...
Supernova
... • Sun-like stars (M< 9 Msolar) stop producing energy with Shell Helium Burning and leave behind a carbon core (White Dwarf). • Stars more massive continue to fuse heavier elements in their cores as they evolve. Carbon burning at 600 Million K Neon burning at 1.2 Billion K Oxygen Burning at 1.5 Billi ...
... • Sun-like stars (M< 9 Msolar) stop producing energy with Shell Helium Burning and leave behind a carbon core (White Dwarf). • Stars more massive continue to fuse heavier elements in their cores as they evolve. Carbon burning at 600 Million K Neon burning at 1.2 Billion K Oxygen Burning at 1.5 Billi ...
Chapter 14
... with different surface temperatures. Note that the peak radiation of a cooler star is more toward the red part of the spectrum, and the peak Radiation of a hotter star is more toward the blue part of the spectrum. ...
... with different surface temperatures. Note that the peak radiation of a cooler star is more toward the red part of the spectrum, and the peak Radiation of a hotter star is more toward the blue part of the spectrum. ...
The Universe
... Brightness of Stars •_____________ ___________ –_____________ ____________ for different _________ of ____________ of objects as __________ _______ ________ ...
... Brightness of Stars •_____________ ___________ –_____________ ____________ for different _________ of ____________ of objects as __________ _______ ________ ...
Disentangling planetary orbits from stellar activity in radial
... Disentangling planetary orbits from stellar activity super-Earth with the smallest measured planetary radius at the time (Leger et al. 2009). This discovery was followed by an intensive RV campaign with HARPS to measure its mass and investigate on the possible presence of other planets (Queloz et a ...
... Disentangling planetary orbits from stellar activity super-Earth with the smallest measured planetary radius at the time (Leger et al. 2009). This discovery was followed by an intensive RV campaign with HARPS to measure its mass and investigate on the possible presence of other planets (Queloz et a ...
Document
... So the spectra reveal details about the light source. We can use that same approach to study planets, stars, and galaxies. We can deduce the temperature and abundances of various chemical elements in the outer atmosphere of a star. Theorists predicted that when the universe was forming there was lit ...
... So the spectra reveal details about the light source. We can use that same approach to study planets, stars, and galaxies. We can deduce the temperature and abundances of various chemical elements in the outer atmosphere of a star. Theorists predicted that when the universe was forming there was lit ...
Unit 1 The Universe
... • Stars form in nebulae. • Nebula -large cloud of gas and dust. It is composed mainly of hydrogen and helium, with small amounts of heavier elements. ...
... • Stars form in nebulae. • Nebula -large cloud of gas and dust. It is composed mainly of hydrogen and helium, with small amounts of heavier elements. ...
L43 THE STARFISH TWINS: TWO YOUNG
... N1 with S4, N2 with S3, and N3 with S1 is equally plausible. A comparison of the fluxes of both PNs at different wavelengths indicates that they are intrinsically similar in size and brightness but are located at different distances. We find that the stellar blue and visual (continuum) fluxes, the H ...
... N1 with S4, N2 with S3, and N3 with S1 is equally plausible. A comparison of the fluxes of both PNs at different wavelengths indicates that they are intrinsically similar in size and brightness but are located at different distances. We find that the stellar blue and visual (continuum) fluxes, the H ...
ppt - Wladimir Lyra
... Runaway Helium burning: 100 billion times the Solar output in just a few seconds ...
... Runaway Helium burning: 100 billion times the Solar output in just a few seconds ...
main-sequence stars
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
... more luminous and have diameters from 10-100 times greater than our sun. Super giants are giant stars that have diameters more than 100 times greater than our sun. These giant stars (but relatively cool) are very luminous. ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.