five minute episode script
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
... DISTINCTIVE BELT OF THREE STARS. IF YOU LOOK A LITTLE CLOSER YOU'LL SEE STARS OF DIFFERENT BRIGHTNESS AND COLOR. DEAN: STAR COLOR IS AN INDICATION OF ITS TEMPERATURE - BLUE STARS BEING THE HOTTEST AND RED STARS BEING THE COLDEST. YOU CAN REALLY SEE THE COLORS OF THE BRIGHTEST STARS LIKE THOSE IN ORI ...
Astronomy 103 – Midterm 2 – October 29, 2014
... 46. Match the phases of stellar evolution listed below (1-4) to the appropriate energy generating processes (A-D). 1 Contraction of the core and fusion of hydrogen to helium in a shell 2 Fusion of helium to carbon in the core 3 Contraction of the entire star 4 Fusion of hydrogen to helium in the cor ...
... 46. Match the phases of stellar evolution listed below (1-4) to the appropriate energy generating processes (A-D). 1 Contraction of the core and fusion of hydrogen to helium in a shell 2 Fusion of helium to carbon in the core 3 Contraction of the entire star 4 Fusion of hydrogen to helium in the cor ...
The Sights of the Deep Sky - Peterborough Astronomical Society
... traviolet part of the spectrum. White and yellow stars are young-tomiddle-aged middleweights. Most of the red stars you can see in the night sky were once massive blue or white stars that now near the end of their lives. Most of the stars of the galaxy are dim red stars, much less massive than our S ...
... traviolet part of the spectrum. White and yellow stars are young-tomiddle-aged middleweights. Most of the red stars you can see in the night sky were once massive blue or white stars that now near the end of their lives. Most of the stars of the galaxy are dim red stars, much less massive than our S ...
Planetary Nebulae – White dwarfs
... • May burn up to carbon but do not have enough mass to get temperatures high enough to go any higher up the periodic table • Degeneracy pressure stops the core from collapsing and heating enough: particles are squashed together as much as possible • End their lives with planetary nebulae, white d ...
... • May burn up to carbon but do not have enough mass to get temperatures high enough to go any higher up the periodic table • Degeneracy pressure stops the core from collapsing and heating enough: particles are squashed together as much as possible • End their lives with planetary nebulae, white d ...
Unit 8 Chapter 30
... from Earth or 32.6 Light years away (10 parsecs). Our sun would be a 4.8, average star, Rigel has an Absolute Magnitude of -6.4 which makes it appear brighter than most stars. Remember, all stars are not the same distance away, therefore, a faint star may really be very bright if it were closer. ...
... from Earth or 32.6 Light years away (10 parsecs). Our sun would be a 4.8, average star, Rigel has an Absolute Magnitude of -6.4 which makes it appear brighter than most stars. Remember, all stars are not the same distance away, therefore, a faint star may really be very bright if it were closer. ...
Galileo Galilei From The Starry Messenger (1610) and The Assayer
... to the unaided vision, adding countless more which have never before been seen, exposing these plainly to the eye in numbers ten times exceeding the old and familiar stars. It is a very beautiful thing, and most gratifying to the sight, to behold the body of the moon, distant from us almost sixty ea ...
... to the unaided vision, adding countless more which have never before been seen, exposing these plainly to the eye in numbers ten times exceeding the old and familiar stars. It is a very beautiful thing, and most gratifying to the sight, to behold the body of the moon, distant from us almost sixty ea ...
c - Fsusd
... 4) The planets and moons in our solar system are visible because they ______. a) emit their own light b) undergo nuclear fusion c) absorb light from the sun d) reflect light from the sun ...
... 4) The planets and moons in our solar system are visible because they ______. a) emit their own light b) undergo nuclear fusion c) absorb light from the sun d) reflect light from the sun ...
THE INCREDIBLE ORIGIN OF THE CHEMICAL ELEMENTS
... cases an enormous explosion (known as a "supernova") results, throwing much of the outer part of the star into space. During it's dying moments, just before it explodes, the temperature of the star rises as high as three billion °C or more. At these temperatures many nuclear process occur which resu ...
... cases an enormous explosion (known as a "supernova") results, throwing much of the outer part of the star into space. During it's dying moments, just before it explodes, the temperature of the star rises as high as three billion °C or more. At these temperatures many nuclear process occur which resu ...
Formation of spiral and elliptical galaxies in a CDM cosmogony
... The attening of the halo (axial ratio 2:3) is too high to be a result of its rotation, i.e., it must be caused by the anisotropic velocity dispersion, while the attening of the bulge (axial ratio 1:1.3) is at least partially due to its rotation (v= 1). These results support the idea that disk ...
... The attening of the halo (axial ratio 2:3) is too high to be a result of its rotation, i.e., it must be caused by the anisotropic velocity dispersion, while the attening of the bulge (axial ratio 1:1.3) is at least partially due to its rotation (v= 1). These results support the idea that disk ...
April 2005
... • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their ...
... • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their ...
Goal: To understand the expansion of our universe.
... • As gas and dust orbits friction causes the gas and dust to heat up, emit light, and fall slowly down towards the object in the center. • If the object in the center is massive you can liberate 10% of the mass energy of the dust and gas as energy (as opposed to 0.7% from fusion). ...
... • As gas and dust orbits friction causes the gas and dust to heat up, emit light, and fall slowly down towards the object in the center. • If the object in the center is massive you can liberate 10% of the mass energy of the dust and gas as energy (as opposed to 0.7% from fusion). ...
Astronomical terms and constants
... 1 AU ≈ 1.5 × 1013 cm = one astronomical unit, i.e. the earth–sun distance. 1 pc = 2.06 × 105 AU = 3.1 × 1018 cm = one parsec, i.e. a distance to a star with a parallax equal to one second of arc. A parallax is an angle at which the radius of earth’s orbit around the sun is seen from a distance of th ...
... 1 AU ≈ 1.5 × 1013 cm = one astronomical unit, i.e. the earth–sun distance. 1 pc = 2.06 × 105 AU = 3.1 × 1018 cm = one parsec, i.e. a distance to a star with a parallax equal to one second of arc. A parallax is an angle at which the radius of earth’s orbit around the sun is seen from a distance of th ...
Lecture Notes – Galaxies
... (2) Non-thermal (synchrotron) emission with excess energy at UV, IR, radio and X-ray wavelengths. (3) Variability over time-scales from few hours to few years – indicates emitting region is few light years across. (4) Often have jets emerging from nucleus. (5) Have emission line spectra. Examples ar ...
... (2) Non-thermal (synchrotron) emission with excess energy at UV, IR, radio and X-ray wavelengths. (3) Variability over time-scales from few hours to few years – indicates emitting region is few light years across. (4) Often have jets emerging from nucleus. (5) Have emission line spectra. Examples ar ...
star - TeacherWeb
... • A star begins as a nebula, a cloud of gas and dust. • 70% hydrogen, 28% helium, 2% heavier elements. • Outside force ( like explosion of star ) compresses cloud of gas, particles move closer to each other and bulled together by gravity. • Regions of dense matter build up • Newton’s Law of Universa ...
... • A star begins as a nebula, a cloud of gas and dust. • 70% hydrogen, 28% helium, 2% heavier elements. • Outside force ( like explosion of star ) compresses cloud of gas, particles move closer to each other and bulled together by gravity. • Regions of dense matter build up • Newton’s Law of Universa ...
Document
... towards the centre of clusters (Solanes+ 2001) • Possible Mechanisms: • Starvation (Larson+ 1980) • Ram pressure stripping (Gunn & Gott 1972) HI in M81 Group of Galaxies (Yun+ 1994) ...
... towards the centre of clusters (Solanes+ 2001) • Possible Mechanisms: • Starvation (Larson+ 1980) • Ram pressure stripping (Gunn & Gott 1972) HI in M81 Group of Galaxies (Yun+ 1994) ...
Stars - Mrs. Tosh`s class
... The entire sky is lit up for weeks. The temperature can be more than 100 billion degrees. The iron atoms fuse into uranium. ...
... The entire sky is lit up for weeks. The temperature can be more than 100 billion degrees. The iron atoms fuse into uranium. ...
Star Planet - Stony Brook Astronomy
... A great collection of stars in space, all held together by gravity and orbiting a common center ...
... A great collection of stars in space, all held together by gravity and orbiting a common center ...
ASTR 105 Intro Astronomy: The Solar System
... image. In looking out into space, we are looking back in time! – The farther away we look in distance, the further back we look in time. ...
... image. In looking out into space, we are looking back in time! – The farther away we look in distance, the further back we look in time. ...
The Life Cycle of a Star
... • Also, they can form when a white dwarf ignites carbon fusion, which results in a runaway nuclear fusion reaction and causes a supernova. • Supernovae can be so immense that the energy produced can equal the energy the Sun creates over a time period of 10 billion years! ...
... • Also, they can form when a white dwarf ignites carbon fusion, which results in a runaway nuclear fusion reaction and causes a supernova. • Supernovae can be so immense that the energy produced can equal the energy the Sun creates over a time period of 10 billion years! ...
Stellar Dynamics
... medium) flows into the centre of the cluster, falling into the gravitational potential well. As a result this gas gets heated up and emits copious amount of X-rays through which it can be observed. Near the centre of rich clusters the gas becomes dense and its cooling time is estimated to be shorter ...
... medium) flows into the centre of the cluster, falling into the gravitational potential well. As a result this gas gets heated up and emits copious amount of X-rays through which it can be observed. Near the centre of rich clusters the gas becomes dense and its cooling time is estimated to be shorter ...
Chapter 34: Cosmology FYI 1. Radar Ranging 2. Triangulation idea
... •Each galaxy started by condensation of huge clouds of hydrogen gas. •Particularly dense regions compressed by gravity to for stars. •Currently our universe is dominated by fusion of hydrogen to form helium. •Structure is stable now, but what happens when hydrogen is used up ...
... •Each galaxy started by condensation of huge clouds of hydrogen gas. •Particularly dense regions compressed by gravity to for stars. •Currently our universe is dominated by fusion of hydrogen to form helium. •Structure is stable now, but what happens when hydrogen is used up ...
mam.mwism
... • Old (~ 11 billion years), lower-main-sequence stars • Approx. 200 globular clusters in our Milky Way ...
... • Old (~ 11 billion years), lower-main-sequence stars • Approx. 200 globular clusters in our Milky Way ...
Measuring Distances - Stockton University
... Due to the spin of the galaxy, an observer will see part of the galaxy approaching them and part of the galaxy running away. This causes the emission from the galaxy to show redshifted, blueshifted, and no-shifted emission. The motion will thus cause a narrow line, e.g., a line due to some element l ...
... Due to the spin of the galaxy, an observer will see part of the galaxy approaching them and part of the galaxy running away. This causes the emission from the galaxy to show redshifted, blueshifted, and no-shifted emission. The motion will thus cause a narrow line, e.g., a line due to some element l ...
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.