THREE INTRIGUER NEBULAE IN CONSTELLATION CARINA
... dozen have been identified up to a distance of 100 Mpc (e.g. Chilingarian et al. 2007, 2009; Price et al. 2009). The prototype of this class is M32 (but see Graham 2002) and their main characteristics are a high central and effective surface brightness for their luminosities, and a high degree of co ...
... dozen have been identified up to a distance of 100 Mpc (e.g. Chilingarian et al. 2007, 2009; Price et al. 2009). The prototype of this class is M32 (but see Graham 2002) and their main characteristics are a high central and effective surface brightness for their luminosities, and a high degree of co ...
Announcements Evolution of High-Mass Stars: Red Supergiants
... • If you get stuck, ask another group for help. • If you get really stuck, raise your hand and I will come around. ...
... • If you get stuck, ask another group for help. • If you get really stuck, raise your hand and I will come around. ...
Lecture 5
... proponent of the so-called "island universes" hypothesis, which holds that spiral nebulae are actually independent galaxies. The matter was conclusively settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of i ...
... proponent of the so-called "island universes" hypothesis, which holds that spiral nebulae are actually independent galaxies. The matter was conclusively settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of i ...
Slide 1
... proponent of the so-called "island universes" hypothesis, which holds that spiral nebulae are actually independent galaxies. The matter was conclusively settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of i ...
... proponent of the so-called "island universes" hypothesis, which holds that spiral nebulae are actually independent galaxies. The matter was conclusively settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of i ...
AST1100 Lecture Notes
... normal ratio, and we have no reason to believe otherwise, then the planets can only explain a tiny part of the invisible matter. Brown dwarf stars (more about these in later lectures) are stars which had too little mass to start nuclear reactions. They emit thermal radiation, but their temperature i ...
... normal ratio, and we have no reason to believe otherwise, then the planets can only explain a tiny part of the invisible matter. Brown dwarf stars (more about these in later lectures) are stars which had too little mass to start nuclear reactions. They emit thermal radiation, but their temperature i ...
powerpoint
... seems to be a “dark matter” in the Universe. If there is enough dark matter, the universe could be “closed,” i.e. it may someday stop expanding and start contracting. 2) Very careful studies of the velocities of galaxies should be able to reveal if the rate of expansion is slowing down. However, the ...
... seems to be a “dark matter” in the Universe. If there is enough dark matter, the universe could be “closed,” i.e. it may someday stop expanding and start contracting. 2) Very careful studies of the velocities of galaxies should be able to reveal if the rate of expansion is slowing down. However, the ...
Small Wonders: Andromeda
... there - especially when you compare it to the two foreground stars that flank it. At mag 13.7, it's a somewhat dim target tho, so the more aperture you can throw at this, the better your chances of finding it. It's certainly doable in a 10" scope from a decent site, and more than likely is catchable ...
... there - especially when you compare it to the two foreground stars that flank it. At mag 13.7, it's a somewhat dim target tho, so the more aperture you can throw at this, the better your chances of finding it. It's certainly doable in a 10" scope from a decent site, and more than likely is catchable ...
Our Galaxy, The Milky Way
... Acceleration of the star moving in a circular orbit must be provided by a net inward gravitational force: ...
... Acceleration of the star moving in a circular orbit must be provided by a net inward gravitational force: ...
The Milky Way Galaxy
... in a galaxy and the formation of the SMBH, but nobody knows what this is. Maybe SMBH are something intrinsic, or even essential, to the process of galaxy formation. ...
... in a galaxy and the formation of the SMBH, but nobody knows what this is. Maybe SMBH are something intrinsic, or even essential, to the process of galaxy formation. ...
understanding-the
... a. A group of people met together and decided to make it a theory. b. There is no other way to explain the formation of the universe. c. Distant galaxies were observed to be moving away from Earth. d. Edwin Hubble was an honest man. ...
... a. A group of people met together and decided to make it a theory. b. There is no other way to explain the formation of the universe. c. Distant galaxies were observed to be moving away from Earth. d. Edwin Hubble was an honest man. ...
Review Sheet and Study Hints - Tufts Institute of Cosmology
... Describe a theory about the formation of spirals. What evidence do we have for that? In what sense is the formation of ellipticals different from that of spirals? In what sense was Hubble correct/incorrect with this evolutionary proposal? How do galaxies in the past look different from gal ...
... Describe a theory about the formation of spirals. What evidence do we have for that? In what sense is the formation of ellipticals different from that of spirals? In what sense was Hubble correct/incorrect with this evolutionary proposal? How do galaxies in the past look different from gal ...
Astronomy Final C - Tarleton State University
... 4. Genetic replication involves A.nucleic acids B.ATP C.amino acids D.genetic replication involves all of these 5. Degenerate gases ? cool without losing their pressure. A.can B.cannot 6. ? develop where supernova explosions leave behind a “core” of approximately 1.4 to 2 or 3 stellar masses. A.Brow ...
... 4. Genetic replication involves A.nucleic acids B.ATP C.amino acids D.genetic replication involves all of these 5. Degenerate gases ? cool without losing their pressure. A.can B.cannot 6. ? develop where supernova explosions leave behind a “core” of approximately 1.4 to 2 or 3 stellar masses. A.Brow ...
81 KB - CSIRO Publishing
... wisdom’, invite readers to vote on their preferred definition of a galaxy via a dedicated website. Keywords: galaxies: dwarf — galaxies: fundamental parameters — galaxies: star clusters — galaxies: general ...
... wisdom’, invite readers to vote on their preferred definition of a galaxy via a dedicated website. Keywords: galaxies: dwarf — galaxies: fundamental parameters — galaxies: star clusters — galaxies: general ...
Disk Galaxies and problem 3
... • Tidal origin of spiral arms. Spiral arms are induced by tidal perturbation of a nearby galaxy. This is observationally seen in grand-design spirals, such as M51. The tidal arms are also easily produced in numerical simulations, see Fig. 7. • Bar spiral arms. A rotating bar at the centre of galaxie ...
... • Tidal origin of spiral arms. Spiral arms are induced by tidal perturbation of a nearby galaxy. This is observationally seen in grand-design spirals, such as M51. The tidal arms are also easily produced in numerical simulations, see Fig. 7. • Bar spiral arms. A rotating bar at the centre of galaxie ...
L6-Diskproperties
... galaxy mass is entirely in stars and gas •assume stellar (bulge/disk) density ~ R-band light and typical M/L •assume gas surface density (disk) is 1.4 x HI intensity •adjust M/L so that gas and stars in disk account for as much of the galaxy’s rotation as possible maximum disk model ...
... galaxy mass is entirely in stars and gas •assume stellar (bulge/disk) density ~ R-band light and typical M/L •assume gas surface density (disk) is 1.4 x HI intensity •adjust M/L so that gas and stars in disk account for as much of the galaxy’s rotation as possible maximum disk model ...
Galactic Evolution:
... There are models with quick pre-enrichment. This includes pre-galactic enrichment, or protogalactic processes, or preenrichment from other more evolved system. ...
... There are models with quick pre-enrichment. This includes pre-galactic enrichment, or protogalactic processes, or preenrichment from other more evolved system. ...
Characteristics of Our Galaxy
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
here
... Defined as the distance from the sun at which two imaginary lines—one projected from the Earth, and one projected from the sun at a right angle to a third line connecting the Earth and the sun—intersect in space at an angle of 1 arcsecond ...
... Defined as the distance from the sun at which two imaginary lines—one projected from the Earth, and one projected from the sun at a right angle to a third line connecting the Earth and the sun—intersect in space at an angle of 1 arcsecond ...
May 2010 - Pomona Valley Amateur Astronomers
... Ron likes to see old photons but the question has been raised, “How old are they?” The first bit of information we need is the redshift, the value of “Z.” What is it? Hydrogen is the most abundant element in the outer reaches of any star. It is simply a proton with an electron orbiting it. Quantum P ...
... Ron likes to see old photons but the question has been raised, “How old are they?” The first bit of information we need is the redshift, the value of “Z.” What is it? Hydrogen is the most abundant element in the outer reaches of any star. It is simply a proton with an electron orbiting it. Quantum P ...
distance to the centre of the Milky Way.
... Herschel (1790) Star Counts He used telescopes to see more stars (since this makes fainter ones visible), but was still just working ‘by eye’. He could not take photographs, for instance. ...
... Herschel (1790) Star Counts He used telescopes to see more stars (since this makes fainter ones visible), but was still just working ‘by eye’. He could not take photographs, for instance. ...
21. Galaxy Evolution Agenda The Monty Hall Problem/Paradox 21.1
... momentum tends to shape a collapsing gas cloud into a spinning disk. Thus, ellipticals may have formed from protogalactic clouds with relatively small amounts of angular momentum, while the clouds that formed spirals had greater angular momentum. (2) Dense clouds tend to cool and form stars more rap ...
... momentum tends to shape a collapsing gas cloud into a spinning disk. Thus, ellipticals may have formed from protogalactic clouds with relatively small amounts of angular momentum, while the clouds that formed spirals had greater angular momentum. (2) Dense clouds tend to cool and form stars more rap ...
Document
... Do you need to learn all of characteristics on RTB’s fine-tuned list to communicate this? No. I have found three characteristics that eliminate all life in the Milky Way and universe, other than earth. 1) Life requires a very stable burning star (sun). To date astronomers have cataloged about 2,500, ...
... Do you need to learn all of characteristics on RTB’s fine-tuned list to communicate this? No. I have found three characteristics that eliminate all life in the Milky Way and universe, other than earth. 1) Life requires a very stable burning star (sun). To date astronomers have cataloged about 2,500, ...
Estimating the mass and star formation rate in galaxies
... during the late stages of stellar evolution regions such as nuclei of galaxies, where many generations of stars are actively forming or have formed, evolved and “died” are often enshrouded by dust which absorbs light. This extinction of light though, depends on the wavel ...
... during the late stages of stellar evolution regions such as nuclei of galaxies, where many generations of stars are actively forming or have formed, evolved and “died” are often enshrouded by dust which absorbs light. This extinction of light though, depends on the wavel ...
SCIN 293-PL-New Course
... Objective 1: Evaluate the lives of galaxies from formation to star production and evolution by collision with other galaxies. Lesson 1: Galactic Evolution Topic 1: The Milky Way Galaxy Topic 2: Formation of Galaxies Topic 3: Active Galactic Nuclei Topic Mastery: Based on the Hubble tuning fork comp ...
... Objective 1: Evaluate the lives of galaxies from formation to star production and evolution by collision with other galaxies. Lesson 1: Galactic Evolution Topic 1: The Milky Way Galaxy Topic 2: Formation of Galaxies Topic 3: Active Galactic Nuclei Topic Mastery: Based on the Hubble tuning fork comp ...
Galaxy Zoo
Galaxy Zoo is a crowdsourced astronomy project which invites people to assist in the morphological classification of large numbers of galaxies. (e.g.) It is an example of citizen science as it enlists the help of members of the public to help in scientific research. There have been seven versions up to July 2014, which are outlined in this article. Galaxy Zoo is part of the Zooniverse, a group of citizen science projects.