Lecture 3
... • Imagine a star with a relatively cool (4000k) atmosphere. Temperature is just a measure of the average velocity of the atoms and molecules in a gas. For a relatively cool gas there are: (1) Few atomic collisions with enough energy to knock electrons up to the 1st excited state so the majority of t ...
... • Imagine a star with a relatively cool (4000k) atmosphere. Temperature is just a measure of the average velocity of the atoms and molecules in a gas. For a relatively cool gas there are: (1) Few atomic collisions with enough energy to knock electrons up to the 1st excited state so the majority of t ...
Mass and the Properties of Main Sequence Stars
... Note: The Mass-Luminosity relation applies to main-sequence stars only! For example, A 10 M⊙ star is roughly (103.5 ~ ) 3,000 brighter, or burning its hydrogen times 3,000 faster. We know that the lifetime of the Sun is about 10 billion years. The more massive star would have a lifetime of abo ...
... Note: The Mass-Luminosity relation applies to main-sequence stars only! For example, A 10 M⊙ star is roughly (103.5 ~ ) 3,000 brighter, or burning its hydrogen times 3,000 faster. We know that the lifetime of the Sun is about 10 billion years. The more massive star would have a lifetime of abo ...
Chapter 13
... 3. T Tauri stars are a certain class of young stars that show rapid and erratic changes in brightness in the form of enormous flares; these flares are thought to play a part in blowing away the cocoon of newly forming stars, particularly K- and M-type stars. 4. M-class stars may remain protostars fo ...
... 3. T Tauri stars are a certain class of young stars that show rapid and erratic changes in brightness in the form of enormous flares; these flares are thought to play a part in blowing away the cocoon of newly forming stars, particularly K- and M-type stars. 4. M-class stars may remain protostars fo ...
Devika kamath Institute of Astronomy, KU. Leuven, Belgium
... circumbinary discs (Van Winckel 2007) ...
... circumbinary discs (Van Winckel 2007) ...
Interstellar medium, birth and life of stars
... star becomes unstable and begins to pulsate. RR Lyrae variables are low-mass, pulsating variables with short periods. Cepheid variables are high-mass, pulsating variables exhibiting a regular relationship between the period of pulsation and luminosity. Mass can be transferred from one star to an ...
... star becomes unstable and begins to pulsate. RR Lyrae variables are low-mass, pulsating variables with short periods. Cepheid variables are high-mass, pulsating variables exhibiting a regular relationship between the period of pulsation and luminosity. Mass can be transferred from one star to an ...
Proficiency Step #5--
... One of the oldest constellations, Ursa Major (ER-suh MAY-jer), The Great Bear is also one of the best known. In particular are the seven stars which make up what is commonly known as the Big Dipper or the Plough. In Cherokee legend, the handle of the Big Dipper represents a team of hunters pursuing ...
... One of the oldest constellations, Ursa Major (ER-suh MAY-jer), The Great Bear is also one of the best known. In particular are the seven stars which make up what is commonly known as the Big Dipper or the Plough. In Cherokee legend, the handle of the Big Dipper represents a team of hunters pursuing ...
All_Stars
... • All stars, regardless of their mass, spend roughly 90% of their total lifetimes as main sequence stars. • Stars end their main sequence lives when their supply of hydrogen fuel runs out in the core. • The most massive stars (O and B types) have very short lifetimes compared to low-mass stars (K an ...
... • All stars, regardless of their mass, spend roughly 90% of their total lifetimes as main sequence stars. • Stars end their main sequence lives when their supply of hydrogen fuel runs out in the core. • The most massive stars (O and B types) have very short lifetimes compared to low-mass stars (K an ...
Constellation
... (from Microsoft ® Encarta ® 2006. © 1993-2005 Microsoft Corporation. All rights reserved) ...
... (from Microsoft ® Encarta ® 2006. © 1993-2005 Microsoft Corporation. All rights reserved) ...
Calculate the Mass of the Milky Way Galaxy
... "cosmic scatter" and is probably due to the fact that the gas clouds that formed the galaxies all had some small additional motion of their own. The recessional velocity of a galaxy at a particular distance inferred from Hubble's law is called the "Hubble velocity". ...
... "cosmic scatter" and is probably due to the fact that the gas clouds that formed the galaxies all had some small additional motion of their own. The recessional velocity of a galaxy at a particular distance inferred from Hubble's law is called the "Hubble velocity". ...
Lesson 4 - Scientist in Residence Program
... Oh, be a fine girl, kiss me!). O and B stars are uncommon but very bright and M stars are common but dull. Astronomers use a diagram (the HertzsprungRussell plot) to graph a star’s colour, temperature, luminosity, spectral type, and evolutionary stage. The largest and brightest stars, the O, B and A ...
... Oh, be a fine girl, kiss me!). O and B stars are uncommon but very bright and M stars are common but dull. Astronomers use a diagram (the HertzsprungRussell plot) to graph a star’s colour, temperature, luminosity, spectral type, and evolutionary stage. The largest and brightest stars, the O, B and A ...
Ch 11c and 12 ( clusters 3-31-11)
... •Contraction and heating of clouds into protostars • Hydrogen fusion stops collapse II. Leaving the Main Sequence: Hydrogen fusion stops 1. Low mass stars (M < 0.4 solar masses) Not enough mass to ever fuse any element heavier than Hydrogen → white dwarf 2.Intermediate mass stars (0.4 solar masses < ...
... •Contraction and heating of clouds into protostars • Hydrogen fusion stops collapse II. Leaving the Main Sequence: Hydrogen fusion stops 1. Low mass stars (M < 0.4 solar masses) Not enough mass to ever fuse any element heavier than Hydrogen → white dwarf 2.Intermediate mass stars (0.4 solar masses < ...
File - Mr. Catt`s Class
... formed red giant will result in the formation of an accretion disk around the white dwarf. The material in the disk comes from the red giant and is mostly hydrogen. 2. An accretion disk is a rotating disk of gas orbiting a star, formed by material falling toward the star. ...
... formed red giant will result in the formation of an accretion disk around the white dwarf. The material in the disk comes from the red giant and is mostly hydrogen. 2. An accretion disk is a rotating disk of gas orbiting a star, formed by material falling toward the star. ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... d, the distance, in order to calculate L. For mass, if it’s a binary star, you can measure the period of the orbit without knowing the distance, but again to get the physical semi-major axis of the orbit from the angular separation of the two stars, you need to know the distance to the system. Prope ...
... d, the distance, in order to calculate L. For mass, if it’s a binary star, you can measure the period of the orbit without knowing the distance, but again to get the physical semi-major axis of the orbit from the angular separation of the two stars, you need to know the distance to the system. Prope ...
CHAPTER 14
... surface (effective) temperature decreases. The star’s position on the H-R diagram moves to the up and right of the main sequence. 3. Massive stars have a greater fusion rate and thus are more luminous. As a result, they can use up the hydrogen in their cores in a few million years. The least massive ...
... surface (effective) temperature decreases. The star’s position on the H-R diagram moves to the up and right of the main sequence. 3. Massive stars have a greater fusion rate and thus are more luminous. As a result, they can use up the hydrogen in their cores in a few million years. The least massive ...
document
... Most large galaxies have a super massive black hole in their center, and most of them are don’t show up either. Galaxies with bigger bulges usually have heavier black holes. ...
... Most large galaxies have a super massive black hole in their center, and most of them are don’t show up either. Galaxies with bigger bulges usually have heavier black holes. ...
Chapter 6 Stars
... brightness of a star can be described in two ways: apparent brightness and absolute brightness. Apparent brightness is how bright the star appears from Earth. Just like a flashlight looks brighter the closer it is to you, a star looks brighter the closer it is to Earth. The sun for instance looks ex ...
... brightness of a star can be described in two ways: apparent brightness and absolute brightness. Apparent brightness is how bright the star appears from Earth. Just like a flashlight looks brighter the closer it is to you, a star looks brighter the closer it is to Earth. The sun for instance looks ex ...
globular cluster - Harding University
... last picture is known, has been visible to observers from ancient times. • The nature of the milky way, however, way was not know until Galileo began to make observations with his telescope. He observed that the Milky Way was a large collection of stars concentrated in a certain region of the sky. • ...
... last picture is known, has been visible to observers from ancient times. • The nature of the milky way, however, way was not know until Galileo began to make observations with his telescope. He observed that the Milky Way was a large collection of stars concentrated in a certain region of the sky. • ...
Betelgeuse
... Apparent Magnitude: 0.50(var.) Absolute Magnitude: -7.2 Distance: ~1400 LY Spectral Type: M1-2Ia-Iab ...
... Apparent Magnitude: 0.50(var.) Absolute Magnitude: -7.2 Distance: ~1400 LY Spectral Type: M1-2Ia-Iab ...
Stellar Evolution
... It can be seen from this H–R diagram that stars more massive than the Sun follow very different paths when leaving the main sequence: ...
... It can be seen from this H–R diagram that stars more massive than the Sun follow very different paths when leaving the main sequence: ...
ON THE FORMATION OF MASSIVE STELLAR CLUSTERS
... As pointed out by Ho (1997) young super-star clusters are overwhelmingly luminous concentrations of stars that present a typical half-light radius of about 3 pc, and a mass that ranges from a few times 104 M to a few 106 M . The brightest ones have luminosities up to two orders of magnitude higher ...
... As pointed out by Ho (1997) young super-star clusters are overwhelmingly luminous concentrations of stars that present a typical half-light radius of about 3 pc, and a mass that ranges from a few times 104 M to a few 106 M . The brightest ones have luminosities up to two orders of magnitude higher ...
DTU_9e_ch13
... The evolutionary tracks of three low-mass supergiants are shown as they eject planetary nebulae. The loops indicate periods of instability and adjustment for the white dwarfs. The dots on this graph represent the central stars of planetary nebulae whose surface temperatures and luminosities have bee ...
... The evolutionary tracks of three low-mass supergiants are shown as they eject planetary nebulae. The loops indicate periods of instability and adjustment for the white dwarfs. The dots on this graph represent the central stars of planetary nebulae whose surface temperatures and luminosities have bee ...
PODEX – PhOtometric Data EXtractor
... All black-box procedures known to us (like IRAF or MOMF) are complicated to handle and provide only the extraction of instrumental magnitudes. For a complete reduction also a color dependent extinction correction and the conversion to relative magnitudes is needed. podex provides it. The podex sourc ...
... All black-box procedures known to us (like IRAF or MOMF) are complicated to handle and provide only the extraction of instrumental magnitudes. For a complete reduction also a color dependent extinction correction and the conversion to relative magnitudes is needed. podex provides it. The podex sourc ...
Stars PowerPoint
... – Although stars may appear to be close to each other, very few are gravitationally bound to one other. – By measuring distances to stars and observing how they interact with each other, scientists can determine which stars are gravitationally bound to each other. – A group of stars that are gravita ...
... – Although stars may appear to be close to each other, very few are gravitationally bound to one other. – By measuring distances to stars and observing how they interact with each other, scientists can determine which stars are gravitationally bound to each other. – A group of stars that are gravita ...
Boötes
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.