of the star. - Colyton High School
... 3. Fusion stops, temperature drops and gas pressure decreases, no longer in equilibrium. 4. Core contracts (gravity WINS by pulling atoms in). 5. Increased temperature (more atoms, more collisions) and gas pressure in the core reinitiates nuclear fusion, equilibrium is achieved, and the cycle begins ...
... 3. Fusion stops, temperature drops and gas pressure decreases, no longer in equilibrium. 4. Core contracts (gravity WINS by pulling atoms in). 5. Increased temperature (more atoms, more collisions) and gas pressure in the core reinitiates nuclear fusion, equilibrium is achieved, and the cycle begins ...
I CAN SEE THE STARS IN YOUR EYES
... Your space craft begins to travel at the speed of light, taking you towards the sun. Traveling at this speed, the trip from Earth to the sun, a distance of 93 million miles, would take about 8 minutes, not very long for such a long trip! Yet, to get to the next closest star, Proxima Centauri, would ...
... Your space craft begins to travel at the speed of light, taking you towards the sun. Traveling at this speed, the trip from Earth to the sun, a distance of 93 million miles, would take about 8 minutes, not very long for such a long trip! Yet, to get to the next closest star, Proxima Centauri, would ...
Astronomy Assignment #1
... luminosity, radius and temperature while on the main sequence, because of the natural thermostat mechanism in main sequence stars. The thermostat mechanism acts to return the core fusion rates back to an equilibrium rate in the event of fluctuations in the core fusion rate. This is known as a negati ...
... luminosity, radius and temperature while on the main sequence, because of the natural thermostat mechanism in main sequence stars. The thermostat mechanism acts to return the core fusion rates back to an equilibrium rate in the event of fluctuations in the core fusion rate. This is known as a negati ...
Galaxies (Professor Powerpoint)
... Mergers can transform two spirals into an elliptical galaxy. Some astronomers think that galaxies are always born as spirals, and they can become ellipticals only via mergers. ...
... Mergers can transform two spirals into an elliptical galaxy. Some astronomers think that galaxies are always born as spirals, and they can become ellipticals only via mergers. ...
HR Diagram Activity - Mr. Alster`s Science Classes
... 10. Overall, are the stars in Group 3 very bright or very dim? 11. Are these stars hot or cool compared to other stars? 12. Is the relationship of brightness to temperature for these stars puzzling, or does it make sense? Explain. Additional Questions 13. As you can see from the Group 1 stars, the ...
... 10. Overall, are the stars in Group 3 very bright or very dim? 11. Are these stars hot or cool compared to other stars? 12. Is the relationship of brightness to temperature for these stars puzzling, or does it make sense? Explain. Additional Questions 13. As you can see from the Group 1 stars, the ...
Parallax, Event Horizon, HR diagrams equation
... Physics : distance to the stars and counting the stars "1 Light Year is the distance traveled by light in one year." 1 light year (ly) is equivalent to: 63,270 AU Closer stars could appear larger. More distant stars could be very large, but seem small. How can we tell which stars are farther away? ...
... Physics : distance to the stars and counting the stars "1 Light Year is the distance traveled by light in one year." 1 light year (ly) is equivalent to: 63,270 AU Closer stars could appear larger. More distant stars could be very large, but seem small. How can we tell which stars are farther away? ...
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2-2 wkst - Home [www.petoskeyschools.org]
... ____________ 22. small hot stars that are dimmer than the sun ____________ 23. high-temperature stars that quickly use up their hydrogen ____________ 24. cool stars with high absolute magnitude ...
... ____________ 22. small hot stars that are dimmer than the sun ____________ 23. high-temperature stars that quickly use up their hydrogen ____________ 24. cool stars with high absolute magnitude ...
Astro 10: Introductory Astronomy
... hydrogen and helium nuclei, and luminosity, all of which have momentum and provide pressure which blow away the surrounding disk of proto-planetary material. Can planets form (thus being dense, stable against this pressure) quickly enough so that the material isn’t simply blown away first? • That’s ...
... hydrogen and helium nuclei, and luminosity, all of which have momentum and provide pressure which blow away the surrounding disk of proto-planetary material. Can planets form (thus being dense, stable against this pressure) quickly enough so that the material isn’t simply blown away first? • That’s ...
The Solar Nebula - Lincoln-Sudbury Regional High School
... (c) How Stars Form Giant molecular clouds are held up by gas pressure, rotation and magnetic fields. If the clouds become massive enough, they can collapse due to gravity. First let’s just consider pressure and gravity: ...
... (c) How Stars Form Giant molecular clouds are held up by gas pressure, rotation and magnetic fields. If the clouds become massive enough, they can collapse due to gravity. First let’s just consider pressure and gravity: ...
Document
... • They are losing mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s. While our own Sun loses approximately 10−14 solar masses every year, Wolf–Rayet stars typically lose 10−5 solar masses a year.[1] • Wolf–Rayet stars are extremely hot, with surface temperatures in th ...
... • They are losing mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s. While our own Sun loses approximately 10−14 solar masses every year, Wolf–Rayet stars typically lose 10−5 solar masses a year.[1] • Wolf–Rayet stars are extremely hot, with surface temperatures in th ...
The Life of a Star
... throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during ...
... throws its outer layers into space, forming a planetary nebula – This leaves behind the hot dense core of the red giant. – The remaining core is called a white dwarf. Over time, the white dwarf cools off and becomes a black dwarf. Planetary Nebula: A collection of gas and dust that was formed during ...
Quantum Well Electron Gain Structures and Infrared
... for life, then there is a limited volume of any stellar system where that might exist – the Habitable Zone • If we assume temperature is dominated by sun/starlight, then the HZ can be calculated for any given star • Likely star types for life are F, G, and K stars (bigger stars die fast; M stars hav ...
... for life, then there is a limited volume of any stellar system where that might exist – the Habitable Zone • If we assume temperature is dominated by sun/starlight, then the HZ can be calculated for any given star • Likely star types for life are F, G, and K stars (bigger stars die fast; M stars hav ...
CARBON STARS
... • Originally classified by Shane (1928) as R and N stars • R0-R3 -> relatively weak C2 and CN bands • R5-R8 -> strong bands and continuum down to 3900Å • N-stars -> also strong bands of C2 and CN but continuum falls off before 4000Å ...
... • Originally classified by Shane (1928) as R and N stars • R0-R3 -> relatively weak C2 and CN bands • R5-R8 -> strong bands and continuum down to 3900Å • N-stars -> also strong bands of C2 and CN but continuum falls off before 4000Å ...
sc_examII_fall_2002 - University of Maryland
... A. a few hundred feet away. B. a few miles away. C. a few hundred miles away. ...
... A. a few hundred feet away. B. a few miles away. C. a few hundred miles away. ...
How many stars are in the Milky Way Galaxy?
... 1: Draw and label diagrams of the Milky Way from top and side views, showing the major components. Indicate the approximate dimensions of the components and note the location of the Sun in each diagram. 2: Describe the galactic distribution of general interstellar material, nebulae, and open and glo ...
... 1: Draw and label diagrams of the Milky Way from top and side views, showing the major components. Indicate the approximate dimensions of the components and note the location of the Sun in each diagram. 2: Describe the galactic distribution of general interstellar material, nebulae, and open and glo ...
The Warrumbungle Observer The Warrumbungle Observer
... Uranus is located 30 degrees lower in the sky than Neptune in Pisces. This appears as a greenish star with a pair of binoculars. The planet has an interesting name, much the joke for some, but has had an identity crisis over the years. Its discoverer William Herschel named it after King George III o ...
... Uranus is located 30 degrees lower in the sky than Neptune in Pisces. This appears as a greenish star with a pair of binoculars. The planet has an interesting name, much the joke for some, but has had an identity crisis over the years. Its discoverer William Herschel named it after King George III o ...
Star Types
... We can “weigh” stars that are in binary systems (two stars orbiting each other). Fortunately, most stars fall into this category. ...
... We can “weigh” stars that are in binary systems (two stars orbiting each other). Fortunately, most stars fall into this category. ...
The Big Bang
... Formation of the Solar System: Solar Nebula – large cloud of dust and gas that formed our solar system.(about 5 billion years ago) As it spun, it flattened like a disk and gravity pulled the solar nebula together to form our sun. ...
... Formation of the Solar System: Solar Nebula – large cloud of dust and gas that formed our solar system.(about 5 billion years ago) As it spun, it flattened like a disk and gravity pulled the solar nebula together to form our sun. ...
Elements from Stardust
... than the sun. • These stars are large enough to produce heavier elements like Magnesium and Silicon. • In Massive stars, fusion continues until the core is almost all iron. ...
... than the sun. • These stars are large enough to produce heavier elements like Magnesium and Silicon. • In Massive stars, fusion continues until the core is almost all iron. ...
Life Cycle of a Star - Intervention Worksheet
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
... A dying red super giant star can suddenly explode. The explosion is called a supernova. After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes whe ...
1 WHY DO THE STARS IN ORION LOOK SO DIFFERENT FROM
... Table 1 is Rigel, with an mv of 0.12, which happens to also be the brightest star in the Orion constellation. The apparent magnitude is as we observe the star from earth. It is not reflective of a stars true physical character, such as its size or luminosity. More on these later. The second stars in ...
... Table 1 is Rigel, with an mv of 0.12, which happens to also be the brightest star in the Orion constellation. The apparent magnitude is as we observe the star from earth. It is not reflective of a stars true physical character, such as its size or luminosity. More on these later. The second stars in ...
Stars: radius and mass
... – There are lines in the spectrum of almost every star. – These lines will be Doppler shifted by the motion of the star in the binary. – The shifts for the two stars will be out of phase, one star is moving towards us as the other is moving away. – Can determine binary nature by looking for motions ...
... – There are lines in the spectrum of almost every star. – These lines will be Doppler shifted by the motion of the star in the binary. – The shifts for the two stars will be out of phase, one star is moving towards us as the other is moving away. – Can determine binary nature by looking for motions ...
3.6 spectral classes
... • Absorption spectra are used to classify stars into nine principal types, called spectral classes. • Hydrogen lines are much stronger in the spectra of some stars than in the Sun’s spectrum. • Astronomers once mistakenly thought that these stars had more hydrogen than other stars. • They classified ...
... • Absorption spectra are used to classify stars into nine principal types, called spectral classes. • Hydrogen lines are much stronger in the spectra of some stars than in the Sun’s spectrum. • Astronomers once mistakenly thought that these stars had more hydrogen than other stars. • They classified ...
What kind of stuff
... • Emission lines arise from gas “ionized” by very energetic radiation • Such high energy radiation is NOT produced by cold old stars, implying that very young stars (10 million years old) are present. • They also contain vast amounts of gas and dust ...
... • Emission lines arise from gas “ionized” by very energetic radiation • Such high energy radiation is NOT produced by cold old stars, implying that very young stars (10 million years old) are present. • They also contain vast amounts of gas and dust ...
Lecture2 - UCSB Physics
... • Emission lines arise from gas “ionized” by very energetic radiation • Such high energy radiation is NOT produced by cold old stars, implying that very young stars (10 million years old) are present. • They also contain vast amounts of gas and dust ...
... • Emission lines arise from gas “ionized” by very energetic radiation • Such high energy radiation is NOT produced by cold old stars, implying that very young stars (10 million years old) are present. • They also contain vast amounts of gas and dust ...
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.