The amazing lives of two stars
... PHASE I: A vast compression wave moves through a galaxy. Spiral shaped, the wave slowly ripples through the galactic disk, and a cosmic traffic jam ensues. As gas encounters this invincible wall of compression, it gets squeezed, forming huge clouds, dark and formidable. Some contain as much matter a ...
... PHASE I: A vast compression wave moves through a galaxy. Spiral shaped, the wave slowly ripples through the galactic disk, and a cosmic traffic jam ensues. As gas encounters this invincible wall of compression, it gets squeezed, forming huge clouds, dark and formidable. Some contain as much matter a ...
The Story of Gold
... hydrogen nuclei (bare protons) into a helium nucleus, a few light sub-atomic particles, and energy. This, and slightly more complex chains with the same result, are the only processes occurring early in a star’s life. Stars go through a series of life stages, each producing heavier elements, governe ...
... hydrogen nuclei (bare protons) into a helium nucleus, a few light sub-atomic particles, and energy. This, and slightly more complex chains with the same result, are the only processes occurring early in a star’s life. Stars go through a series of life stages, each producing heavier elements, governe ...
Earth in the Universe
... evolves to next depends on their original mass. • Stars with masses similar to our sun expand to become red giants. When the red giant uses up its nuclear fuel it collapses into a white dwarf and then a black dwarf. ...
... evolves to next depends on their original mass. • Stars with masses similar to our sun expand to become red giants. When the red giant uses up its nuclear fuel it collapses into a white dwarf and then a black dwarf. ...
Surface Environments of the Planets o+ our Solar System
... In this exercise, you will also become more familiar with the various naming systems for stars. Remember, only the brightest stars which form our constellations have been given proper names. There are thousands of stars that have either Bayer Greek letter names, and even more that have Flamsteed num ...
... In this exercise, you will also become more familiar with the various naming systems for stars. Remember, only the brightest stars which form our constellations have been given proper names. There are thousands of stars that have either Bayer Greek letter names, and even more that have Flamsteed num ...
Brichler-powerpoint
... relationship between the surface temperature and the absolute brightness of stars. • (see page 114) ...
... relationship between the surface temperature and the absolute brightness of stars. • (see page 114) ...
Unit 1
... • c. always emits the same spectrum of light, whatever its temperature • d. reflects all radiation which falls upon it, never heating up and always appearing black. ...
... • c. always emits the same spectrum of light, whatever its temperature • d. reflects all radiation which falls upon it, never heating up and always appearing black. ...
Ourdraft
... Young Stars in IC 2118 We are studying a nebula (cloud of gas and dust) called Interstellar Cloud 2118, or the Witch Head Nebula, that is being excited by a young, very hot star called Rigel. Because Rigel is so energetic, it sends off shock waves that hit the nebula, compressing some of the gas (at ...
... Young Stars in IC 2118 We are studying a nebula (cloud of gas and dust) called Interstellar Cloud 2118, or the Witch Head Nebula, that is being excited by a young, very hot star called Rigel. Because Rigel is so energetic, it sends off shock waves that hit the nebula, compressing some of the gas (at ...
Observation
... Large concentration of electromagnetic radiation in small region of space with small fraction of baryons Sudden release of high intensity gammarays produces e+e- pairs which create an ...
... Large concentration of electromagnetic radiation in small region of space with small fraction of baryons Sudden release of high intensity gammarays produces e+e- pairs which create an ...
Stars - Robert M. Hazen
... Great Ideas in Science: Lecture 8 – Stars & Galaxies Professor Robert Hazen UNIV 301 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star’s nuclear fuel is depleted, the star must burn out. ...
... Great Ideas in Science: Lecture 8 – Stars & Galaxies Professor Robert Hazen UNIV 301 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star’s nuclear fuel is depleted, the star must burn out. ...
Star Classification - University of Louisville
... An old Blue-white star becomes a Supergiant. They expand, just like average-sized stars expand to become Giant stars. Because they are beginning to run out of hydrogen, they cool down and glow a more orangey color. A star called Betelguese is extremely old, but also extremely big. In fact, it is 500 ...
... An old Blue-white star becomes a Supergiant. They expand, just like average-sized stars expand to become Giant stars. Because they are beginning to run out of hydrogen, they cool down and glow a more orangey color. A star called Betelguese is extremely old, but also extremely big. In fact, it is 500 ...
Characteristics of Stars Stars Analyzing Starlight Star Characteristics
... · spectrographs - device that separates light into different wavelengths (colors) · each star produces a unique spectrum (series of colors and lines) · a star's spectrum tells us elements present (composition) surface temperature how fast the star is moving toward or away from Earth ...
... · spectrographs - device that separates light into different wavelengths (colors) · each star produces a unique spectrum (series of colors and lines) · a star's spectrum tells us elements present (composition) surface temperature how fast the star is moving toward or away from Earth ...
doc - IAC
... massive. They stand out because of their high luminosity. These stars can become a million times brighter than the Sun. Their masses can be measured dynamically, in the same way as planetary masses are measured. The most massive ones are 100 to 150 times heavier than the Sun. The most massive stars ...
... massive. They stand out because of their high luminosity. These stars can become a million times brighter than the Sun. Their masses can be measured dynamically, in the same way as planetary masses are measured. The most massive ones are 100 to 150 times heavier than the Sun. The most massive stars ...
Stars Part 2 - westscidept
... • 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 light years away. There are thousands of closer stars in the sky that we do not se ...
... • 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 light years away. There are thousands of closer stars in the sky that we do not se ...
Gemini
... cubic parsec. Some authors have estimated a larger diameter of up to 46' (H. Shapley in 1930). With about 100 million years (WEBDA gives a value 95, the Sky Catalogue 2000.0 of 110 million years), it is of intermediate age, and contains some post-main sequence stars (including several yellow and ora ...
... cubic parsec. Some authors have estimated a larger diameter of up to 46' (H. Shapley in 1930). With about 100 million years (WEBDA gives a value 95, the Sky Catalogue 2000.0 of 110 million years), it is of intermediate age, and contains some post-main sequence stars (including several yellow and ora ...
Powerpoint
... Why is the gas ionized? Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are form ...
... Why is the gas ionized? Remember, takes energetic UV photons to ionize H. Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are form ...
Universe Notes - Solon City Schools
... a. Main sequence: A line or sequence in an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
... a. Main sequence: A line or sequence in an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
Announcements
... jumps up to a higher level, or when an electron in a higher level emits a photon and jumps down to the 2nd level. ...
... jumps up to a higher level, or when an electron in a higher level emits a photon and jumps down to the 2nd level. ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.