Variables, Star Clusters, and Nebulae (Professor Powerpoint)
... giving off visible light (red in color) ...
... giving off visible light (red in color) ...
The Life CyCLe of STarS - Origins
... 33 Star Birth. The atoms produced by the previous generation of stars become part of a new generation. New stars called nebulae are formed inside rich clouds of gas and dust (see photo next page). Within this stellar nursery, a small dense pocket of gas and dust begins to collapse under gravity. Thi ...
... 33 Star Birth. The atoms produced by the previous generation of stars become part of a new generation. New stars called nebulae are formed inside rich clouds of gas and dust (see photo next page). Within this stellar nursery, a small dense pocket of gas and dust begins to collapse under gravity. Thi ...
Test #4 (Ch. 13-16) ASTR 10 You have 1 hour to take the exam, and
... C. The cloud must radiate much of its thermal energy. D. The cloud must trap most of its thermal energy. 4. Consider a large molecular cloud that will give birth to a cluster of stars. Which of the following would you expect to be true? A. All the stars in the cluster will become main-sequence stars ...
... C. The cloud must radiate much of its thermal energy. D. The cloud must trap most of its thermal energy. 4. Consider a large molecular cloud that will give birth to a cluster of stars. Which of the following would you expect to be true? A. All the stars in the cluster will become main-sequence stars ...
Star formation Stars form out of dense, cold, often dusty, molecular
... Summary: star formation on large scales 1) Stars form out of molecular gas which is assembled into dense molecular clouds in spiral arms. 2) Molecular clouds have a complex, often filamentary structure. Individual stars, or small groups, form from the smallest scale structures, cloud cores of size ...
... Summary: star formation on large scales 1) Stars form out of molecular gas which is assembled into dense molecular clouds in spiral arms. 2) Molecular clouds have a complex, often filamentary structure. Individual stars, or small groups, form from the smallest scale structures, cloud cores of size ...
20081 Study Guide_77-120
... To help students understand how astronomers can infer the existence of black holes, use the example of two ice skaters holding hands and spinning in a circle. If one of the skaters were invisible, an observer could still infer that two skaters were present by observing the effect the invisible skate ...
... To help students understand how astronomers can infer the existence of black holes, use the example of two ice skaters holding hands and spinning in a circle. If one of the skaters were invisible, an observer could still infer that two skaters were present by observing the effect the invisible skate ...
stars
... • Stars change over their lifespan just like animals change throughout their life. • Nebula-a large cloud of gas and dust spread out over a large volume of space. • They can have different appearances bright or dark ...
... • Stars change over their lifespan just like animals change throughout their life. • Nebula-a large cloud of gas and dust spread out over a large volume of space. • They can have different appearances bright or dark ...
A Brief History of Planetary Science
... If we take a spectrum of a star, what does it look like? ...
... If we take a spectrum of a star, what does it look like? ...
Main-sequence stars - Stellar Populations
... connect some of those ideas together By Marc Rafelski Parts of this are © 2006 Pearson Education Inc, publishing as Addison-Wesley ...
... connect some of those ideas together By Marc Rafelski Parts of this are © 2006 Pearson Education Inc, publishing as Addison-Wesley ...
Stars
... • A star is a ball of plasma held together by its own gravity – Nuclear reactions occur in stars (H He) – Energy from the nuclear reactions is released as electromagnetic radiation • They look small because they are a long way away, but in fact many are bigger and brighter than our Sun. • The heat ...
... • A star is a ball of plasma held together by its own gravity – Nuclear reactions occur in stars (H He) – Energy from the nuclear reactions is released as electromagnetic radiation • They look small because they are a long way away, but in fact many are bigger and brighter than our Sun. • The heat ...
Star formation slides
... Herbig-Haro objects: important signposts of starformation. Outflows/jets ejected at few 100s km/s impact the surrounding ISM and ionize it, making the jets visible. The jet creates bow-shocks, where the supersonic flow collides with the stationary ambient gas. In reality, the jet ‘lights up’ severa ...
... Herbig-Haro objects: important signposts of starformation. Outflows/jets ejected at few 100s km/s impact the surrounding ISM and ionize it, making the jets visible. The jet creates bow-shocks, where the supersonic flow collides with the stationary ambient gas. In reality, the jet ‘lights up’ severa ...
STARS
... that can last for weeks and reach 40,000 km high. • Solar Flare: Like a solar prominence, but the gases travel into the corona, and last only a few minutes. ...
... that can last for weeks and reach 40,000 km high. • Solar Flare: Like a solar prominence, but the gases travel into the corona, and last only a few minutes. ...
Study Guide
... Black hole - spinning causes the core to collapse allowing nothing to escape Neutron star - the left over core of a supernova that begins to rotate very fast Explain the Doppler shift in terms of color and direction. If an object is moving away from us, the color spectra will shift toward red Red ...
... Black hole - spinning causes the core to collapse allowing nothing to escape Neutron star - the left over core of a supernova that begins to rotate very fast Explain the Doppler shift in terms of color and direction. If an object is moving away from us, the color spectra will shift toward red Red ...
IL CIELO COME LABORATORIO – 2010/2011 STAR FORMATION
... difference of about 1 Mpc between the closest and the furthest arm of the galaxy. The mean quantity of ionizing photons is 8·1049, that is also the amount of the ionized gas. The number of stars which belong to O5 spectral class, needed to warm all the ionized gas is nearly 12 stars. In the same way ...
... difference of about 1 Mpc between the closest and the furthest arm of the galaxy. The mean quantity of ionizing photons is 8·1049, that is also the amount of the ionized gas. The number of stars which belong to O5 spectral class, needed to warm all the ionized gas is nearly 12 stars. In the same way ...
Classifying Stars - Concord Academy Boyne
... of years. These small stars die quietly, and in their place, a small white dwarf is left behind. ...
... of years. These small stars die quietly, and in their place, a small white dwarf is left behind. ...
So why are more massive stars more luminous?
... with TAs by sending them e-mail, starting now. The first 50 will be signed up for March 7. If there are more then 50 people they will be signed up for ...
... with TAs by sending them e-mail, starting now. The first 50 will be signed up for March 7. If there are more then 50 people they will be signed up for ...
Lecture21 - UCSB Physics
... converted into helium, the core has contracted a bit, and the Sun’s luminosity has gone up by about 40%. These changes in the core have made the Sun’s outer layers expand in radius by 6% and increased the surface temperature from 5500 K to 5800 K. ...
... converted into helium, the core has contracted a bit, and the Sun’s luminosity has gone up by about 40%. These changes in the core have made the Sun’s outer layers expand in radius by 6% and increased the surface temperature from 5500 K to 5800 K. ...
Integrative Studies 410 Our Place in the Universe
... pressure due to heat generated (outward) • Stars neither shrink nor expand, they are in hydrostatic equilibrium, i.e. the forces are equally strong ...
... pressure due to heat generated (outward) • Stars neither shrink nor expand, they are in hydrostatic equilibrium, i.e. the forces are equally strong ...
ppt
... Analysing spectra gave rise to the subject of Astrophysics. Previously astronomy was just about categorising objects based on their appearance (morphology). But by studying their spectra, we can use physical models to understand their nature. Many of these astronomical objects just appear as dots in ...
... Analysing spectra gave rise to the subject of Astrophysics. Previously astronomy was just about categorising objects based on their appearance (morphology). But by studying their spectra, we can use physical models to understand their nature. Many of these astronomical objects just appear as dots in ...
ppt
... The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it’s own pressure. To understand how this simple system behaves, however, requires an understanding of: ...
... The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it’s own pressure. To understand how this simple system behaves, however, requires an understanding of: ...
Life and fate of a star
... a star like our Sun. The outer layers of the star were ejected four thousand years ago, and their fading red glow is now slowly moving away from the white dwarf. The stellar remnant still emits some ultraviolet light, which bathes the central area of the nebula. This is how the future of our Sun may ...
... a star like our Sun. The outer layers of the star were ejected four thousand years ago, and their fading red glow is now slowly moving away from the white dwarf. The stellar remnant still emits some ultraviolet light, which bathes the central area of the nebula. This is how the future of our Sun may ...
Scientists classify stars by
... The gravity of a passing star or the shock wave from a nearby supernova may cause the nebula to contract. 1. Matter in the gas cloud will begin to come together into a dense region called a protostar. 2. As the protostar continues to condense, it heats up. 3. Eventually, it reaches a critical mass a ...
... The gravity of a passing star or the shock wave from a nearby supernova may cause the nebula to contract. 1. Matter in the gas cloud will begin to come together into a dense region called a protostar. 2. As the protostar continues to condense, it heats up. 3. Eventually, it reaches a critical mass a ...
Stars Part 2 - westscidept
... • How bright a star looks in the sky from Earth is called apparent magnitude. • A dim star might look bright to us on Earth if it is close. At the same time, we may barely be able to see a very bright star if it is too far away. • Betelgeuse which is one of the brightest stars in the sky is 310 lig ...
... • How bright a star looks in the sky from Earth is called apparent magnitude. • A dim star might look bright to us on Earth if it is close. At the same time, we may barely be able to see a very bright star if it is too far away. • Betelgeuse which is one of the brightest stars in the sky is 310 lig ...
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.