The Sun is a mass of Incandescent Gas
... 14N + 1H --> 15O + photon – 15O = (8 p + 7 n) 15O --> 15N + antielectron + neutrino – 15N = (7 p + 8 n) 15N + 1H --> 12C + 4He ...
... 14N + 1H --> 15O + photon – 15O = (8 p + 7 n) 15O --> 15N + antielectron + neutrino – 15N = (7 p + 8 n) 15N + 1H --> 12C + 4He ...
Space Science Unit
... phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). They make up 90% of the stars in our sky. These stars are the diagonal strip running through the middle of the chart. ...
... phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). They make up 90% of the stars in our sky. These stars are the diagonal strip running through the middle of the chart. ...
H-R Diagram - SFA Physics
... Now plot all the stars from Table 7 onto Figure 3. Table 7 is a list of the 30 stars nearest the sun and the majority of these stars are considered to be the most common types of stars in the galaxy. Transfer the main sequence curve from Figure 1 to Figure 3. ...
... Now plot all the stars from Table 7 onto Figure 3. Table 7 is a list of the 30 stars nearest the sun and the majority of these stars are considered to be the most common types of stars in the galaxy. Transfer the main sequence curve from Figure 1 to Figure 3. ...
Document
... • Mass of Sun • Radius of Earth • Hot as Sun’s core • A million times denser than lead • Slowly cool off ...
... • Mass of Sun • Radius of Earth • Hot as Sun’s core • A million times denser than lead • Slowly cool off ...
Our Community`s Place Among the Stars
... years •small, cooler stars live twice as long •massive, supergiant stars consume their mass too quickly only live a few tens of million of years •very hot stars go through their fuel very quickly ...
... years •small, cooler stars live twice as long •massive, supergiant stars consume their mass too quickly only live a few tens of million of years •very hot stars go through their fuel very quickly ...
2010_02_04 LP08 Our Galactic Home
... Lasers (reflecting off the Moon) Radar (reflecting off the Moon or Venus) Heliocentric parallax (Earth’s ORBIT as baseline) Moving clusters (Pleiades) H-R Diagram R R Lyrae variable stars (M=0.5) Cepheid variable stars Brightest supergiants (M=-8) “Normal” novae Globular clusters (brightest at M=-10 ...
... Lasers (reflecting off the Moon) Radar (reflecting off the Moon or Venus) Heliocentric parallax (Earth’s ORBIT as baseline) Moving clusters (Pleiades) H-R Diagram R R Lyrae variable stars (M=0.5) Cepheid variable stars Brightest supergiants (M=-8) “Normal” novae Globular clusters (brightest at M=-10 ...
Stellar Evolution - Hays High Indians
... form – More massive stars can completely form in a few hundred thousand years ...
... form – More massive stars can completely form in a few hundred thousand years ...
Life Cycle of a Star - CullenScience
... Now, for whichever hypothesis you chose, type a 1-3 sentence explanation for why you think this is so. 3. __________ stars have more fuel, but they have to burn (fuse) it faster in order to maintain equilibrium. Therefore, ____________stars live longer than __________ stars because their rate of fue ...
... Now, for whichever hypothesis you chose, type a 1-3 sentence explanation for why you think this is so. 3. __________ stars have more fuel, but they have to burn (fuse) it faster in order to maintain equilibrium. Therefore, ____________stars live longer than __________ stars because their rate of fue ...
Star Formation, HR Diagram, and the Main Sequence (Professor
... Radial velocities are measured using the Doppler Shift of the star's spectrum: •Star moving towards Earth: Blueshift •Star moving away from Earth: Redshift •Star moving across our line of sight: No Shift In all cases, the Radial Velocity is Independent of Distance. ...
... Radial velocities are measured using the Doppler Shift of the star's spectrum: •Star moving towards Earth: Blueshift •Star moving away from Earth: Redshift •Star moving across our line of sight: No Shift In all cases, the Radial Velocity is Independent of Distance. ...
Life Cycle of a Star - Intervention Worksheet
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
... After a low or medium mass or star becomes a red giant, the outer parts grow bigger and drift into space, forming a cloud of gas called a planetary nebula. The blue-white hot core of the star that is left behind cools and becomes a white dwarf. The white dwarf eventually runs out of fuel and dies as ...
Life Cycle of Stars
... core collapses and the rest of the star starts to collapse in after it, but then it bounces off. There is a huge shock wave and in just a second: BANG! 20. The outer parts of this massive star are blasted off into space in a huge Supernova explosion. 21. These Supernova explosions are so powerful th ...
... core collapses and the rest of the star starts to collapse in after it, but then it bounces off. There is a huge shock wave and in just a second: BANG! 20. The outer parts of this massive star are blasted off into space in a huge Supernova explosion. 21. These Supernova explosions are so powerful th ...
No Slide Title
... of an object due to the movement of the observer. Remember looking at your finger through the left and then right eye? One parsec is the distance an object must be in order to have a parallax of one arc second. One parsec = 3.3 light years Alpha Centauri is the closest star. Most stars are too dista ...
... of an object due to the movement of the observer. Remember looking at your finger through the left and then right eye? One parsec is the distance an object must be in order to have a parallax of one arc second. One parsec = 3.3 light years Alpha Centauri is the closest star. Most stars are too dista ...
The HR Diagram Interpreted (PowerPoint version)
... …we discover that Sirius B is just as massive as the sun. But we know it is somewhat smaller than the Earth (to explain its limited brightness) A simple calculation then reveals that ‘Sirius B’ is ...
... …we discover that Sirius B is just as massive as the sun. But we know it is somewhat smaller than the Earth (to explain its limited brightness) A simple calculation then reveals that ‘Sirius B’ is ...
CONSTELLATION URSA MAJOR, THE GREAT
... Ursa Major (also known as the Great Bear) is a constellation in the northern celestial hemisphere. It was one of the 48 constellations listed by Ptolemy (second century AD), and remains one of the 88 modern constellations. It can be visible throughout the year in most of the northern hemisphere. Its ...
... Ursa Major (also known as the Great Bear) is a constellation in the northern celestial hemisphere. It was one of the 48 constellations listed by Ptolemy (second century AD), and remains one of the 88 modern constellations. It can be visible throughout the year in most of the northern hemisphere. Its ...
The HR Diagram Interpreted: Properties of Stars
... …we discover that Sirius B is just as massive as the sun. But we know it is somewhat smaller than the Earth (to explain its limited brightness) A simple calculation then reveals that ‘Sirius B’ is one million times as dense as water - a tonne per cubic cm There is nothing on Earth like this. This is ...
... …we discover that Sirius B is just as massive as the sun. But we know it is somewhat smaller than the Earth (to explain its limited brightness) A simple calculation then reveals that ‘Sirius B’ is one million times as dense as water - a tonne per cubic cm There is nothing on Earth like this. This is ...
ref H-R Spectral types
... In this Activity we have had a look at the Balmer series, and how its occurrence in the photospheres of stars will vary with temperature. The temperature, and hence the colour and spectral line strength characteristics of stars, is used to classify them into types O, B, A, F, G, K and M-type stars. ...
... In this Activity we have had a look at the Balmer series, and how its occurrence in the photospheres of stars will vary with temperature. The temperature, and hence the colour and spectral line strength characteristics of stars, is used to classify them into types O, B, A, F, G, K and M-type stars. ...
Star- large ball of gas held together by large ball of gas held
... Sun The sun is a mass of incandescent gas, a gigantic nuclear furnace. Where hydrogen is built into helium at a temperature of millions of degrees. ...
... Sun The sun is a mass of incandescent gas, a gigantic nuclear furnace. Where hydrogen is built into helium at a temperature of millions of degrees. ...
Unit 1
... on the left. Energy level diagrams of these elements are shown on the right. Which energy level diagram corresponds to absorption line 1 located at 1? 7. The Sun has been fusing hydrogen into helium for about 4.6 billion years now. How much has the amount of helium on the surface (i.e., in the phot ...
... on the left. Energy level diagrams of these elements are shown on the right. Which energy level diagram corresponds to absorption line 1 located at 1? 7. The Sun has been fusing hydrogen into helium for about 4.6 billion years now. How much has the amount of helium on the surface (i.e., in the phot ...
PDF version (two pages, including the full text)
... At about 40 times the diameter of the sun and 400 times as bright, Alphard is one of the ‘bright giants’ in our neighborhood. But our ‘neighborhood’ 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 ov ...
... At about 40 times the diameter of the sun and 400 times as bright, Alphard is one of the ‘bright giants’ in our neighborhood. But our ‘neighborhood’ 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 ov ...
Stars
... BLUE, the COLDEST stars are RED. (Note- this is opposite to what we are used to associating with temperature.) • Color is used to determine ages – stages – in life cycle. ...
... BLUE, the COLDEST stars are RED. (Note- this is opposite to what we are used to associating with temperature.) • Color is used to determine ages – stages – in life cycle. ...
Lars Bildsten - nnpss
... The luminosity of the star is determined by heat transport, since the core is hot, and the surface is cold (VACUUM!). Unlike in your house, the heat is transported by diffusion of photons, which have a mean free path l, giving: ...
... The luminosity of the star is determined by heat transport, since the core is hot, and the surface is cold (VACUUM!). Unlike in your house, the heat is transported by diffusion of photons, which have a mean free path l, giving: ...
Slide 1
... collide and eventually form a single galaxy. • So much space between the stars that they ...
... collide and eventually form a single galaxy. • So much space between the stars that they ...
PowerPoint - Star Life Cycle
... to occur quickly. – This causes the largest stars to burn their fuel, and eventually run out, much more quickly Larger stars live shorter lives. Bigger stars are brighter and hotter due to the rapid rate of fusion. ...
... to occur quickly. – This causes the largest stars to burn their fuel, and eventually run out, much more quickly Larger stars live shorter lives. Bigger stars are brighter and hotter due to the rapid rate of fusion. ...
OBAFGKM
... Cecelia figured out WHY stellar spectra are so different: TEMPERATURE • She showed that SURFACE TEMPERATURE is the big factor • She used the newly-devised SAHA EQUATION that could estimate how many electrons remain attached to atoms as temperature is changed (or the level of ionization) ...
... Cecelia figured out WHY stellar spectra are so different: TEMPERATURE • She showed that SURFACE TEMPERATURE is the big factor • She used the newly-devised SAHA EQUATION that could estimate how many electrons remain attached to atoms as temperature is changed (or the level of ionization) ...
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.