Earth
... hydrogen (about 70%) and helium (about 28%). Carbon, nitrogen and oxygen make up 1.5% and the other 0.5% is made up of small amounts of many other elements such as neon, iron, silicon, magnesium and sulfur. The sun shines because it is burning hydrogen into helium in its extremely hot core. This mea ...
... hydrogen (about 70%) and helium (about 28%). Carbon, nitrogen and oxygen make up 1.5% and the other 0.5% is made up of small amounts of many other elements such as neon, iron, silicon, magnesium and sulfur. The sun shines because it is burning hydrogen into helium in its extremely hot core. This mea ...
Cosmic Dawn A Hunting for the First Stars in the Universe
... of these secondary elements backwards in time, we can infer the existence of generations of stars that have long since disappeared, in much the same way that an archeologist peels back geological strata to map the fossil record of extinct species. What astronomers call the “pollution” of the univer ...
... of these secondary elements backwards in time, we can infer the existence of generations of stars that have long since disappeared, in much the same way that an archeologist peels back geological strata to map the fossil record of extinct species. What astronomers call the “pollution” of the univer ...
1 Astronomical Measurements and Quantities 2 Astronomical Objects
... Distance Ladder: The Hubble low (V=HD) and the expansion of the Universe. The Baade-Wesselink method. A brief overview of different methods treated through the course to go from very nearby objects to very distant ones. [K],[BM] Galaxy Clusters: Morphological classification. Main properties. Cluster ...
... Distance Ladder: The Hubble low (V=HD) and the expansion of the Universe. The Baade-Wesselink method. A brief overview of different methods treated through the course to go from very nearby objects to very distant ones. [K],[BM] Galaxy Clusters: Morphological classification. Main properties. Cluster ...
File - Science with Mrs. Schmidt
... b. some of the colors and some black lines. c. all the colors. d. all the colors and some black lines. _____ 11. What instrument breaks a star’s light into a spectrum? a. a continuous spectrum b. a telescope c. a spectrometer d. a spectrograph _____ 12. What can scientists tell about a star from its ...
... b. some of the colors and some black lines. c. all the colors. d. all the colors and some black lines. _____ 11. What instrument breaks a star’s light into a spectrum? a. a continuous spectrum b. a telescope c. a spectrometer d. a spectrograph _____ 12. What can scientists tell about a star from its ...
CHAPTER 2 NOTES (STARS AND GALAXIES)
... 3 types of galaxies are: 1. spiral- arms like a pinwheel ex our galaxy- Milky Way 2. elliptical- nearly spherical to flatdisks (older than other galaxies) 3. irregular- no orderly or definite shape, not very common Milky Way Galaxy- pinwheel shaped disk with bulge in center -the older stars are near ...
... 3 types of galaxies are: 1. spiral- arms like a pinwheel ex our galaxy- Milky Way 2. elliptical- nearly spherical to flatdisks (older than other galaxies) 3. irregular- no orderly or definite shape, not very common Milky Way Galaxy- pinwheel shaped disk with bulge in center -the older stars are near ...
Document
... radio waves from the VLA (purple), optical data from Hubble (yellow and blue), and infrared with Spitzer (red). NGC 4258 is well known to astronomers for having "anomalous" arms that are not aligned with the plane of the galaxy, but rather intersect ...
... radio waves from the VLA (purple), optical data from Hubble (yellow and blue), and infrared with Spitzer (red). NGC 4258 is well known to astronomers for having "anomalous" arms that are not aligned with the plane of the galaxy, but rather intersect ...
Document
... luminosities and different temperatures. • Stars have different sizes. • If you know: ...
... luminosities and different temperatures. • Stars have different sizes. • If you know: ...
Slide 1
... We calculated the age to be between 12 to 14 billion years old It is 25,000 light years away from Earth ...
... We calculated the age to be between 12 to 14 billion years old It is 25,000 light years away from Earth ...
Our Universe
... •The surface of a black hole is known as the event horizon. This is not a normal surface that you could see or touch. At the event horizon, the pull of gravity becomes infinitely strong. Thus, an object can exist there for only an instant as it plunges inward at the speed of light. ...
... •The surface of a black hole is known as the event horizon. This is not a normal surface that you could see or touch. At the event horizon, the pull of gravity becomes infinitely strong. Thus, an object can exist there for only an instant as it plunges inward at the speed of light. ...
What`s Up - April 2016
... At about 40 times the diameter of the sun and 400 times as bright, Alphard is one of the ‘bright giants’ in our neighbourhood. But our ‘neighbourhood’ is rather large. Alphard is 11 million times as far away from us as our own sun – so it looks a lot dimmer to us! To the south of Sirius, and nearly ...
... At about 40 times the diameter of the sun and 400 times as bright, Alphard is one of the ‘bright giants’ in our neighbourhood. But our ‘neighbourhood’ is rather large. Alphard is 11 million times as far away from us as our own sun – so it looks a lot dimmer to us! To the south of Sirius, and nearly ...
stars
... it starts to burn fuel and glow. • The star burns out it’s fuel it glows less and begins to expand. This star is called a Red Giant. • The star will eventually collapse and explode this is know as the Supernova stage.(only the ones much bigger than our sun – 8 x or more) • Depending on it’s size it ...
... it starts to burn fuel and glow. • The star burns out it’s fuel it glows less and begins to expand. This star is called a Red Giant. • The star will eventually collapse and explode this is know as the Supernova stage.(only the ones much bigger than our sun – 8 x or more) • Depending on it’s size it ...
The Stellar Luminosity Function
... visual magnitude and r is the distance in parsecs . Since the table gives the distances in light years, the formula had to be modified to M =m+5-5 logD/3.26 . Th e absolute magnitudes were then rounded to the nearest whole magnitude and then plotted. (See fig.1 .) The sun's absolute magnitude is 4.8 ...
... visual magnitude and r is the distance in parsecs . Since the table gives the distances in light years, the formula had to be modified to M =m+5-5 logD/3.26 . Th e absolute magnitudes were then rounded to the nearest whole magnitude and then plotted. (See fig.1 .) The sun's absolute magnitude is 4.8 ...
Aspire: Star Life Cycle - Easy Peasy All-in
... 20. Choose a hypothesis and then continue. 21. Where would you expect to find other main sequence stars of the same size on this diagram? (2 Points) 22. Which description of the relationship is correct? (2 Points) 23. Write down the hypothesis that is correct. (2 Points) 24. Determine if the followi ...
... 20. Choose a hypothesis and then continue. 21. Where would you expect to find other main sequence stars of the same size on this diagram? (2 Points) 22. Which description of the relationship is correct? (2 Points) 23. Write down the hypothesis that is correct. (2 Points) 24. Determine if the followi ...
Sep 2017 - What`s Out Tonight?
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
... cury, Venus, Mars, Jupiter and Saturn. Venus is extremely bright Open clusters reside in our Milky Way Galaxy. Our Sun is no and hugs close to the Sun, so you see it for a short time in the longer in its group. west after sunset or in the east before sunrise. Jupiter can be out Globular Clusters loo ...
Andromeda and the Local Group Lesson Plan
... Way, and we’ll take a closer look at some of the nebula inside galaxies that are orbiting our own. Show the video. Review what they saw: ...
... Way, and we’ll take a closer look at some of the nebula inside galaxies that are orbiting our own. Show the video. Review what they saw: ...
Brighter than the average star?
... Small and dim M type stars seem to be the most common stars in space, at least in our part of the Milky Way. Of the 100 closest stars to the Sun, 80 are red dwarfs, and the vast majority of these cannot be seen with the naked eye. The average red dwarf radiates only 4% as much energy as the Sun. The ...
... Small and dim M type stars seem to be the most common stars in space, at least in our part of the Milky Way. Of the 100 closest stars to the Sun, 80 are red dwarfs, and the vast majority of these cannot be seen with the naked eye. The average red dwarf radiates only 4% as much energy as the Sun. The ...
Stars Notes
... 4.b – Students know that the Sun is one of many stars in the Milky Way galaxy and that stars may differ in size, temperature and color 4.d – Students know that stars are the source of light for all bright objects in outer space and that the Moon and planets shine by reflected sunlight, not by thei ...
... 4.b – Students know that the Sun is one of many stars in the Milky Way galaxy and that stars may differ in size, temperature and color 4.d – Students know that stars are the source of light for all bright objects in outer space and that the Moon and planets shine by reflected sunlight, not by thei ...
Endpoints of Stellar Evolution
... In a massive star, core temperature can be high enough that nuclear burning of Si to Fe can occur. Beyond Fe, further fusion is endothermic, and will not occur under equilibrium conditions. As an iron core develops, other reactions still proceed at larger ...
... In a massive star, core temperature can be high enough that nuclear burning of Si to Fe can occur. Beyond Fe, further fusion is endothermic, and will not occur under equilibrium conditions. As an iron core develops, other reactions still proceed at larger ...
Stellar Clusters and Star Formation:
... namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and observed that the actual process of the formation individual stars of conside ...
... namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and observed that the actual process of the formation individual stars of conside ...
powerpoint - Physics @ IUPUI
... • On the plus side, the accretion disk goes down to a few km in size at which point the gas has been heated quite a bit (infalling gas is slowed by frictional heating and interactions with the magnetic field). • The innermost parts will emit X-rays! ...
... • On the plus side, the accretion disk goes down to a few km in size at which point the gas has been heated quite a bit (infalling gas is slowed by frictional heating and interactions with the magnetic field). • The innermost parts will emit X-rays! ...
ISP 205: Visions of the Universe Fall 2001 Professor: ER Capriotti
... 75. The Chandrasekhar limit implies that stars ending up more massive than 1.4 solar masses cannot become A. giant stars B. supernovae C. neutron stars D. black holes E. white dwarfs 76. Black holes are A. places where no matter can exist. B. places where gravity prevents light from escaping. ...
... 75. The Chandrasekhar limit implies that stars ending up more massive than 1.4 solar masses cannot become A. giant stars B. supernovae C. neutron stars D. black holes E. white dwarfs 76. Black holes are A. places where no matter can exist. B. places where gravity prevents light from escaping. ...
Why do some galaxies stop making new stars?
... have lifetimes of just 30 million years. spiral galaxies without star formation, utilising In cosmological terms, 30 million years is a blink of images from NASA's Wide-field Infrared Survey Explorer. the eye. Find a galaxy with these blue stars, and you are seeing a galaxy forming stars (or that We ...
... have lifetimes of just 30 million years. spiral galaxies without star formation, utilising In cosmological terms, 30 million years is a blink of images from NASA's Wide-field Infrared Survey Explorer. the eye. Find a galaxy with these blue stars, and you are seeing a galaxy forming stars (or that We ...
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.