University of Groningen Mass loss and rotational CO emission
... evolved stars were obtained during several observing periods between April 2000 and September 2002 using the James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii. For this purpose, all five different heterodyne receivers available at the JCMT were used, including the new MPIfR/SRON E-band recei ...
... evolved stars were obtained during several observing periods between April 2000 and September 2002 using the James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii. For this purpose, all five different heterodyne receivers available at the JCMT were used, including the new MPIfR/SRON E-band recei ...
- National Optical Astronomy Observatory
... sequence appears to lie around NGC 1496-1. This star’s color index is approximately 0.062, classifying it as a spectral type A star. Based on this observation, the age of the cluster is estimated to be no greater than 400 million years. Stars 21 and 46 appear to be outliers in the data set. This cou ...
... sequence appears to lie around NGC 1496-1. This star’s color index is approximately 0.062, classifying it as a spectral type A star. Based on this observation, the age of the cluster is estimated to be no greater than 400 million years. Stars 21 and 46 appear to be outliers in the data set. This cou ...
Quiz 2 Lecture 12
... a. Ring galaxies can be produced by head-on collisions between galaxies. b. The ratio of the number of elliptical to spiral galaxies remains constant over time. c. The Magellanic Clouds may eventually be "cannibalized" by our Galaxy. d. The shape of a galaxy can be influenced by collision with anoth ...
... a. Ring galaxies can be produced by head-on collisions between galaxies. b. The ratio of the number of elliptical to spiral galaxies remains constant over time. c. The Magellanic Clouds may eventually be "cannibalized" by our Galaxy. d. The shape of a galaxy can be influenced by collision with anoth ...
The Zodiac - Alchemical.org
... Pleiades: An open cluster of stars, clearly visible to the naked eye. It is estimated to contain between 300 and 500 members within a sphere 30 light years across, and is 400 light years away. The stars are embedded in a reflection nebula of cold gas and dust that appears blue in colour photographs. ...
... Pleiades: An open cluster of stars, clearly visible to the naked eye. It is estimated to contain between 300 and 500 members within a sphere 30 light years across, and is 400 light years away. The stars are embedded in a reflection nebula of cold gas and dust that appears blue in colour photographs. ...
Basic Properties of the Stars
... will last only 30 million years. A star with 0.25 solar masses can last 320 billion years. Hot stars are blue, and soon they are through.... ...
... will last only 30 million years. A star with 0.25 solar masses can last 320 billion years. Hot stars are blue, and soon they are through.... ...
Participant Handout - Math Machines Home
... wavelength of a star’s peak emission as described by the equation: λmax T= 3,000,000 nm K The actual brightness (luminosity) of a star is determined by the star’s size and temperature. In addition to having a more bluish color, higher temperature stars emit a larger quantity of light. Still, there a ...
... wavelength of a star’s peak emission as described by the equation: λmax T= 3,000,000 nm K The actual brightness (luminosity) of a star is determined by the star’s size and temperature. In addition to having a more bluish color, higher temperature stars emit a larger quantity of light. Still, there a ...
SPECTRAL ANALYSIS OF A NEWLY DISCOVERED HgMn STAR
... age ~100Myr) open cluster, using low and high-resolution (R~7500, R~25000) spectra stretching from 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star wer ...
... age ~100Myr) open cluster, using low and high-resolution (R~7500, R~25000) spectra stretching from 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star wer ...
Assignment 7 - Department of Physics and Astronomy
... rotate the most rapidly. But the stars are all very far away, so none of them can be seen to spin even when he looks through the largest telescopes. How then can he identify the stars that rotate rapidly? a. all stars that rotate show a huge Doppler shift toward the blue end of the spectrum b. star ...
... rotate the most rapidly. But the stars are all very far away, so none of them can be seen to spin even when he looks through the largest telescopes. How then can he identify the stars that rotate rapidly? a. all stars that rotate show a huge Doppler shift toward the blue end of the spectrum b. star ...
Published by the Association Pro ISSI No. 37, May 2016
... of giant nebulae that are large interstellar clouds of dust, hydrogen, helium and other ionized gases, (Fig. 2) . These clouds are really huge, they may measure several light years across. They are not stable in the long run; rather, internal turbulences cause knots to form which then collapse under ...
... of giant nebulae that are large interstellar clouds of dust, hydrogen, helium and other ionized gases, (Fig. 2) . These clouds are really huge, they may measure several light years across. They are not stable in the long run; rather, internal turbulences cause knots to form which then collapse under ...
Astronomy - Scioly.org
... 23. All stars are composed of mostly hydrogen and helium, yet many stars have no lines for hydrogen or helium in their spectrum. What causes this apparent contradiction? a. Spectral lines are created in the lower atmospheres of stars, and for many stars hydrogen and helium are hidden below the atmo ...
... 23. All stars are composed of mostly hydrogen and helium, yet many stars have no lines for hydrogen or helium in their spectrum. What causes this apparent contradiction? a. Spectral lines are created in the lower atmospheres of stars, and for many stars hydrogen and helium are hidden below the atmo ...
here - Stars `r` Us!
... interstellar medium. However, when this reservoir is empty, a galaxy has little opportunity for further development and can only await the death of the stars that it contains. The interstellar medium of galaxies is replenished to some extent by material expelled from stars in winds and explosions, s ...
... interstellar medium. However, when this reservoir is empty, a galaxy has little opportunity for further development and can only await the death of the stars that it contains. The interstellar medium of galaxies is replenished to some extent by material expelled from stars in winds and explosions, s ...
Ay 112 Midterm review
... Depending on the temperature, different ionization states are present and lines have different strengths in the spectrum. This gives us another way to determine the photospheric temperature (besides Wiens law ...
... Depending on the temperature, different ionization states are present and lines have different strengths in the spectrum. This gives us another way to determine the photospheric temperature (besides Wiens law ...
Glossary Topics - Home - DMNS Galaxy Guide Portal
... The lifecycle of a star depends mostly on the initial mass of the star, though chemical makeup and interactions with companion stars can also have a profound effect. (Most stars are born in double and multiple star systems.) The following is a basic outline: ...
... The lifecycle of a star depends mostly on the initial mass of the star, though chemical makeup and interactions with companion stars can also have a profound effect. (Most stars are born in double and multiple star systems.) The following is a basic outline: ...
Publisher: Emily Barrosse Acquisitions Editor: Kelley Tyner
... creating a visible shell (Fig. 13–2). Each of these two models has its proponents, and observations are being carried out to discover which is valid in most cases. In any case, we know of a thousand such shells of gas in our galaxy. Each shell contains about 20 per cent of the Sun’s mass. They are e ...
... creating a visible shell (Fig. 13–2). Each of these two models has its proponents, and observations are being carried out to discover which is valid in most cases. In any case, we know of a thousand such shells of gas in our galaxy. Each shell contains about 20 per cent of the Sun’s mass. They are e ...
The Sun and other Stars
... Bright cool stars are called ___________________. Red giants are large stars. They are very bright because they are very big, but are also relatively cool. They appear red because of their low temperature. They are in the upper right corner of the H-R diagram. (page 379) Gas giants have relatively _ ...
... Bright cool stars are called ___________________. Red giants are large stars. They are very bright because they are very big, but are also relatively cool. They appear red because of their low temperature. They are in the upper right corner of the H-R diagram. (page 379) Gas giants have relatively _ ...
talk.wyse - Johns Hopkins University
... chemical evolution) despite similar dark matter haloes – constrains ‘feedback’ and effects on DM Adds to challenges for CDM: need to consider a variety of DM candidates e.g. STERILE NEUTRINOS ...
... chemical evolution) despite similar dark matter haloes – constrains ‘feedback’ and effects on DM Adds to challenges for CDM: need to consider a variety of DM candidates e.g. STERILE NEUTRINOS ...
The Solar System and Beyond
... 5. Ask the students to predict how long it would take to run or walk 63,360 inches. 6. Explain that since an inch is so small compared to the total distance being measured, it is hard to imagine how far 63,360 inches is. For this reason, it is difficult to predict how long it would take to run that ...
... 5. Ask the students to predict how long it would take to run or walk 63,360 inches. 6. Explain that since an inch is so small compared to the total distance being measured, it is hard to imagine how far 63,360 inches is. For this reason, it is difficult to predict how long it would take to run that ...
Constellation Argo Navis
... 1751. The Carina Nebula overall is a colossal emission nebula approximately quest for the Golden Fleece. 8,000 light-years away and 300 light-years wide that possesses vast star-forming regions; it has an overall magnitude of 8.0 and a massive apparent diameter, more than 2 degrees. Its central regi ...
... 1751. The Carina Nebula overall is a colossal emission nebula approximately quest for the Golden Fleece. 8,000 light-years away and 300 light-years wide that possesses vast star-forming regions; it has an overall magnitude of 8.0 and a massive apparent diameter, more than 2 degrees. Its central regi ...
Physics-Y11-LP3 - All Saints` Catholic High School
... LP4/3 • explain how data about supernovae can be used to estimate distances to other galaxies • use data to plot a graph of velocity against distance and get a value of the Hubble constant • appreciate that, as new data is collected, the value for the Hubble constant is reviewed • use a spreadsheet ...
... LP4/3 • explain how data about supernovae can be used to estimate distances to other galaxies • use data to plot a graph of velocity against distance and get a value of the Hubble constant • appreciate that, as new data is collected, the value for the Hubble constant is reviewed • use a spreadsheet ...
Separating Stars and Galaxies Based on Color
... If a high resolution spectrum is available for an object, star/galaxy classification is almost always trivial, as spectral features unique to stars or galaxies are easily identifiable. However, due to limitations in telescope time and current detector technology, we do not have a spectrum for each o ...
... If a high resolution spectrum is available for an object, star/galaxy classification is almost always trivial, as spectral features unique to stars or galaxies are easily identifiable. However, due to limitations in telescope time and current detector technology, we do not have a spectrum for each o ...
My talk on CO at z=0 from Santiago in June, 2011
... A Preview of the Next 10 Years (‘10s) ALMA! Maturation of Wide-Field Receivers, Big Surveys An ALMA preview: the PAWS Survey (PI: E. Schinnerer) – PDBI 1” (50 pc) Map of M51: ...
... A Preview of the Next 10 Years (‘10s) ALMA! Maturation of Wide-Field Receivers, Big Surveys An ALMA preview: the PAWS Survey (PI: E. Schinnerer) – PDBI 1” (50 pc) Map of M51: ...
O star
... spectral type and the luminosity class of a star from its spectrum. This is extraordinarily valuable, as it means that, just from the spectrum of a star, one can plot it in on the H-R diagram. BUT: if you can plot a star on the H-R diagram, you know its absolute magnitude! And if you know its absolu ...
... spectral type and the luminosity class of a star from its spectrum. This is extraordinarily valuable, as it means that, just from the spectrum of a star, one can plot it in on the H-R diagram. BUT: if you can plot a star on the H-R diagram, you know its absolute magnitude! And if you know its absolu ...
Celestial Distances - Wayne State University
... changes when its temperature and size change pressure from hot gas ...
... changes when its temperature and size change pressure from hot gas ...
The Sun and other Stars
... relatively cool. They appear red because of their low temperature. They are in the upper right corner of the H-R diagram. (page 379) Gas giants have relatively low densities ...
... relatively cool. They appear red because of their low temperature. They are in the upper right corner of the H-R diagram. (page 379) Gas giants have relatively low densities ...
Virtual Sky II (Rev 10/11)
... (Size of star on chart related to brightness but look at magnitude in data panel to be sure. Lowest magnitude is brightest) Name of a double star ____________ (Click on brighter stars. If it is double there will be a components tab on the data panel) Name and number of a Messier object in the conste ...
... (Size of star on chart related to brightness but look at magnitude in data panel to be sure. Lowest magnitude is brightest) Name of a double star ____________ (Click on brighter stars. If it is double there will be a components tab on the data panel) Name and number of a Messier object in the conste ...
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.