The Milky Way - TCNJ | The College of New Jersey
... • Some of these are compressed enough to form bright O-B STAR CLUSTERS, which can in turn ionize and light up parts of the clouds into H II regions. • Stars older than about 20-30 Myr are usually outside the arms. • NOTE: the arms are barely denser in stars than the rest of the disk but they stand o ...
... • Some of these are compressed enough to form bright O-B STAR CLUSTERS, which can in turn ionize and light up parts of the clouds into H II regions. • Stars older than about 20-30 Myr are usually outside the arms. • NOTE: the arms are barely denser in stars than the rest of the disk but they stand o ...
Chapter 19. Mapping the Universe from Herschel to Sloan
... The key to understanding the nature of galaxies was to get their distances. In the mid1920’s telescopes were able to resolve individual stars in the closest galaxies, such as M31 (Andromeda Galaxy) and M33, but the star were too faint to obtain spectra which could be classified. Therefore, we did no ...
... The key to understanding the nature of galaxies was to get their distances. In the mid1920’s telescopes were able to resolve individual stars in the closest galaxies, such as M31 (Andromeda Galaxy) and M33, but the star were too faint to obtain spectra which could be classified. Therefore, we did no ...
Universe 8e Lecture Chapter 24 Galaxies
... A rich cluster contains hundreds or even thousands of galaxies; a poor cluster, often called a group, may contain only a few dozen. A regular cluster has a nearly spherical shape with a central concentration of galaxies; in an irregular cluster, galaxies are distributed asymmetrically. ...
... A rich cluster contains hundreds or even thousands of galaxies; a poor cluster, often called a group, may contain only a few dozen. A regular cluster has a nearly spherical shape with a central concentration of galaxies; in an irregular cluster, galaxies are distributed asymmetrically. ...
ASTRONOMY AND ASTROPHYSICS Letter to the Editor Low
... The sky frames have been computed using between 15 and 37 subsequent exposures per waveband and night, and careful eyeinspection showed that all sources have been efficiently removed using our modified median filtering technique which returns the lower 1/3 instead of the mean (1/2) value. We subtrac ...
... The sky frames have been computed using between 15 and 37 subsequent exposures per waveband and night, and careful eyeinspection showed that all sources have been efficiently removed using our modified median filtering technique which returns the lower 1/3 instead of the mean (1/2) value. We subtrac ...
Chapter 17
... showing our own Sun's position and Shapley's distribution of these clusters. 2. Which are more useful in mapping the spiral structure of the Milky Way, H-I or H-II regions? Explain why in terms of the electromagnetic spectrum. 3. William Herschel made the first attempt to map our position in the Mil ...
... showing our own Sun's position and Shapley's distribution of these clusters. 2. Which are more useful in mapping the spiral structure of the Milky Way, H-I or H-II regions? Explain why in terms of the electromagnetic spectrum. 3. William Herschel made the first attempt to map our position in the Mil ...
Binocular Universe: Summer`s Swan Song
... binoculars its way and you’ll find not one, but two suns. Fourth-magnitude Omicron-1 will appear pale orange, while its 5th-magnitude companion, 30 Cygni, is blue-white. Defocusing your binoculars slightly will enhance the colors, but keep them sharp to spot a third member, a 7th-magnitude sun just ...
... binoculars its way and you’ll find not one, but two suns. Fourth-magnitude Omicron-1 will appear pale orange, while its 5th-magnitude companion, 30 Cygni, is blue-white. Defocusing your binoculars slightly will enhance the colors, but keep them sharp to spot a third member, a 7th-magnitude sun just ...
Our Galaxy, the Milky Way Galaxy
... Super bubbles will grow (and move more ISM) when the O and B stars go supernova Remember, the gas is still moving around randomly! o The ISM is frothy (some parts are thicker/denser than others via randomness) o Diffuse nebula – More DENSE area of ISM surrounded by a less dense area of ISM Cal ...
... Super bubbles will grow (and move more ISM) when the O and B stars go supernova Remember, the gas is still moving around randomly! o The ISM is frothy (some parts are thicker/denser than others via randomness) o Diffuse nebula – More DENSE area of ISM surrounded by a less dense area of ISM Cal ...
Friday03
... • Fraction of SF galaxies depends on local and large-scale densities (?) • Galaxy-galaxy interactions are the most likely cause of observed segregation ...
... • Fraction of SF galaxies depends on local and large-scale densities (?) • Galaxy-galaxy interactions are the most likely cause of observed segregation ...
The Milky Way Galaxy
... • Surveys of Giant Molecular Clouds (GMCs) are likely to trace the spiral arms since these are sites of star formation • positions interior to Sun’s orbit in Galaxy have some distance ambiguity •Less distance ambiguity outside of Solar orbit, and better evidence of arm-like morphology ...
... • Surveys of Giant Molecular Clouds (GMCs) are likely to trace the spiral arms since these are sites of star formation • positions interior to Sun’s orbit in Galaxy have some distance ambiguity •Less distance ambiguity outside of Solar orbit, and better evidence of arm-like morphology ...
MilkyWay
... • Surveys of Giant Molecular Clouds (GMCs) are likely to trace the spiral arms since these are sites of star formation • positions interior to Sun’s orbit in Galaxy have some distance ambiguity •Less distance ambiguity outside of Solar orbit, and better evidence of arm-like morphology ...
... • Surveys of Giant Molecular Clouds (GMCs) are likely to trace the spiral arms since these are sites of star formation • positions interior to Sun’s orbit in Galaxy have some distance ambiguity •Less distance ambiguity outside of Solar orbit, and better evidence of arm-like morphology ...
about Stars
... 0.1 times as much fuel, uses it 0.01 times as fast 100 billion years ~ 10 billion years x 0.1 / 0.01 ...
... 0.1 times as much fuel, uses it 0.01 times as fast 100 billion years ~ 10 billion years x 0.1 / 0.01 ...
Down Under from North Florida
... Nebula or the magnificent 47 Tucanae globular cluster. Yet with careful planning, several interesting and beautiful southern sky objects can be found in far southern skies. For example, the sky’s second brightest appearing star, Canopus (Alpha Carinae), remains invisible from most of USA locations. ...
... Nebula or the magnificent 47 Tucanae globular cluster. Yet with careful planning, several interesting and beautiful southern sky objects can be found in far southern skies. For example, the sky’s second brightest appearing star, Canopus (Alpha Carinae), remains invisible from most of USA locations. ...
The Milky Way
... So Can Stochastic Star Formation • Random birth of Massive Stars • Their SN explosions compress nearby clouds & make new stars • Differential rotation of galaxy yields spiral appearance by streching the stars out • This best explains "rattier", broken-up spirals (like the Milky Way, though some Den ...
... So Can Stochastic Star Formation • Random birth of Massive Stars • Their SN explosions compress nearby clouds & make new stars • Differential rotation of galaxy yields spiral appearance by streching the stars out • This best explains "rattier", broken-up spirals (like the Milky Way, though some Den ...
Question 1
... b) The rotation of the bulge and disk components c) The Sun’s age and age of the globular cluster stars d) The motion of spiral arms and the mass of the central black hole e) The orbital period and distance from the Galactic center of objects near the edge of the Galaxy Explanation: Use the modified ...
... b) The rotation of the bulge and disk components c) The Sun’s age and age of the globular cluster stars d) The motion of spiral arms and the mass of the central black hole e) The orbital period and distance from the Galactic center of objects near the edge of the Galaxy Explanation: Use the modified ...
The extragalactic universe and distance measurements
... – Tried to determine distribution of stars in Milky Way – described Milky Way as “detached nebula”, with Sun near center. – Thought that the nebulae could be similar systems – Turns out that his conclusions were heavily effected by dust in the Milky Way – Milky Way is much bigger and better ordered ...
... – Tried to determine distribution of stars in Milky Way – described Milky Way as “detached nebula”, with Sun near center. – Thought that the nebulae could be similar systems – Turns out that his conclusions were heavily effected by dust in the Milky Way – Milky Way is much bigger and better ordered ...
2.1 Introduction
... When completed, the current ESA Space Astrometry Mission, Gaia, launched in December 2013, will be a major leap forward: • Positional accuracy: from 0.001 arcsec to 0.00001 arcsec (×102 ) • Distance: from 1 kpc to 100 kpc, sufficient to reach stars in neighbouring galaxies! • Sensitivity: from 10 ma ...
... When completed, the current ESA Space Astrometry Mission, Gaia, launched in December 2013, will be a major leap forward: • Positional accuracy: from 0.001 arcsec to 0.00001 arcsec (×102 ) • Distance: from 1 kpc to 100 kpc, sufficient to reach stars in neighbouring galaxies! • Sensitivity: from 10 ma ...
ASTR 101 Scale of the Universe: an Overview
... Can we see all of the Milky way galaxy from Earth? What is the reason we see Milky way as a luminous cloud? What is most distant object in the universe one can see without a telescope? What are the dark areas in the Milky way we see, devoid of any stars? What are the Magellanic clouds? What is the s ...
... Can we see all of the Milky way galaxy from Earth? What is the reason we see Milky way as a luminous cloud? What is most distant object in the universe one can see without a telescope? What are the dark areas in the Milky way we see, devoid of any stars? What are the Magellanic clouds? What is the s ...
ASTR2100 - Saint Mary's University | Astronomy & Physics
... In 1837 Argelander, of the Bonn Observatory and orginator of the BD catalogue, was able to derive an apex for the solar motion from studying stellar proper motions. His result is very similar to that recognized today. Also in 1837, Frederick Struve found evidence for interstellar extinction in star ...
... In 1837 Argelander, of the Bonn Observatory and orginator of the BD catalogue, was able to derive an apex for the solar motion from studying stellar proper motions. His result is very similar to that recognized today. Also in 1837, Frederick Struve found evidence for interstellar extinction in star ...
Lecture 9a: More on Star formation and evolution 10/22
... classes (O B A F G K M)… – Spectral classes are correlated with temperature, that is determined from the peak wavelength of “blackbody” ...
... classes (O B A F G K M)… – Spectral classes are correlated with temperature, that is determined from the peak wavelength of “blackbody” ...
The birth and life of stars
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
Powerpoint
... when part of a dust cloud begins to contract under its own gravitational force (remember, stars are ~1020 x denser than a molecular cloud). As it collapses, the center becomes hotter and hotter until nuclear fusion begins in the core. Probably new molecular clouds form continually out of less dense ...
... when part of a dust cloud begins to contract under its own gravitational force (remember, stars are ~1020 x denser than a molecular cloud). As it collapses, the center becomes hotter and hotter until nuclear fusion begins in the core. Probably new molecular clouds form continually out of less dense ...
Chapter 14 The Milky Way Galaxy
... galaxy would have to be outside the visible part to reproduce the observed curve. ...
... galaxy would have to be outside the visible part to reproduce the observed curve. ...
Disks around low-mass stars in extreme environments
... comes from winds of evolved stars, or supernovae (M✶ ≤ 30 M⊙) ...
... comes from winds of evolved stars, or supernovae (M✶ ≤ 30 M⊙) ...
Star Formation
... Star Formation Stars that are nearing the main sequence are ejecting gases These stars are in the final stages of birth They are known as T-Taurus stars These blown off gases clear the area surrounding the star ...
... Star Formation Stars that are nearing the main sequence are ejecting gases These stars are in the final stages of birth They are known as T-Taurus stars These blown off gases clear the area surrounding the star ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.