Space Science Chapter 4 Reading Guide BIG IDEA: Our Sun is
... 4. How do stars form inside a nebula? ...
... 4. How do stars form inside a nebula? ...
Great Migrations & other natural history tales
... Medieval theories: The pendulum starts swinging Aristotle's work rediscovered in 13th century, starts Renaissance in Europe. For 100 years everybody agrees with him on most issues. Roger Bacon (1214-1292) at Oxford cites the argument about the impossibility of vacuum between the planetary systems. ...
... Medieval theories: The pendulum starts swinging Aristotle's work rediscovered in 13th century, starts Renaissance in Europe. For 100 years everybody agrees with him on most issues. Roger Bacon (1214-1292) at Oxford cites the argument about the impossibility of vacuum between the planetary systems. ...
Hubble space photos
... • 5000 light-years from Earth • ring is formed of comet-shaped objects moving away from a dying star ...
... • 5000 light-years from Earth • ring is formed of comet-shaped objects moving away from a dying star ...
Our Place in the Universe: Sizing up the Heavens
... The Doppler Effect applied to light – Spectrum of approaching stars is shifted to shorter wave-length (blue shift) whereas receding stars experience red shift. The faster the relative motion, the greater the shift. Amazingly, almost all stars in the Universe are red ...
... The Doppler Effect applied to light – Spectrum of approaching stars is shifted to shorter wave-length (blue shift) whereas receding stars experience red shift. The faster the relative motion, the greater the shift. Amazingly, almost all stars in the Universe are red ...
Abstract Submitted for the PHY599 Meeting of
... for star clusters, but cannot be applied to isolated (field-) stars. A short description of the ”Isochrone method” for determining a star’s age will be given. Finally a recently developed method, the ”Gyrochronology”, will be explained in detail. If there is time, I will also show a technique based ...
... for star clusters, but cannot be applied to isolated (field-) stars. A short description of the ”Isochrone method” for determining a star’s age will be given. Finally a recently developed method, the ”Gyrochronology”, will be explained in detail. If there is time, I will also show a technique based ...
4.1 – 4.3 - s3.amazonaws.com
... »Group of stars outlining an imaginary picture »most have been identified since ancient times »Constellations were once used to navigate by travelers because they appear to revolve around the North Star »They are also used to refer to 88 regions of the sky (celestial sphere) ...
... »Group of stars outlining an imaginary picture »most have been identified since ancient times »Constellations were once used to navigate by travelers because they appear to revolve around the North Star »They are also used to refer to 88 regions of the sky (celestial sphere) ...
Astronomy Name Formation of the Solar System Directions: Use the
... ____ Icy matter and cooler gases settled on the outside of the disk where it was cooler. Planets such as______________ formed from this. ____ The disk grew thinner as the solar nebula continued spinning. ____ The solar nebula began spinning and _____________. ____ The explosion made waves that squee ...
... ____ Icy matter and cooler gases settled on the outside of the disk where it was cooler. Planets such as______________ formed from this. ____ The disk grew thinner as the solar nebula continued spinning. ____ The solar nebula began spinning and _____________. ____ The explosion made waves that squee ...
This chapter has a brief overview of astronomical topics that we will
... years. A more massive star lives a hotter, shorter life. In a few billion years the core of the sun will contract and the outer layers expand. It will expand almost to the orbit of the earth, ending all life on our planet. This is the red giant phase (the outer layers cool as the great size overmatc ...
... years. A more massive star lives a hotter, shorter life. In a few billion years the core of the sun will contract and the outer layers expand. It will expand almost to the orbit of the earth, ending all life on our planet. This is the red giant phase (the outer layers cool as the great size overmatc ...
[WC 6] nucleus with other emission-lines nuclei of planetary nebulae
... stars, are very likely helium burning, formed, else along post-AGB helium-burning tracks, or after a late thermal pulse occured during the post-PN cooling phase and pushing the star back to the PN regime. At the present time, it is not possible to decide if, for a given PN, the first or the second s ...
... stars, are very likely helium burning, formed, else along post-AGB helium-burning tracks, or after a late thermal pulse occured during the post-PN cooling phase and pushing the star back to the PN regime. At the present time, it is not possible to decide if, for a given PN, the first or the second s ...
Life Cycle of Stars - Lab Science Schedule
... When massive stars are formed, they usually have at least six times as much mass as the sun. Massive stars start out like medium sized stars and continue on the same life-cycle until they become red giants. Then they take a much different path. Gravity continues to pull together the carbon atoms in ...
... When massive stars are formed, they usually have at least six times as much mass as the sun. Massive stars start out like medium sized stars and continue on the same life-cycle until they become red giants. Then they take a much different path. Gravity continues to pull together the carbon atoms in ...
Final Exam Study Guide
... Draw the HR Diagram. Put the spectral sequence on the bottom and match it roughly with temperature. Also point out the different luminosity classes (I, II, III, IV, V…). What is a type V star called? Would you find a hydrogen burning core in a type II star? Where are the most luminous stars? How doe ...
... Draw the HR Diagram. Put the spectral sequence on the bottom and match it roughly with temperature. Also point out the different luminosity classes (I, II, III, IV, V…). What is a type V star called? Would you find a hydrogen burning core in a type II star? Where are the most luminous stars? How doe ...
Evolution of a Low-Mass Star
... "Planetary Nebulae" - Low mass star (< 8 Msun) cannot achieve 600 Million K temp. needed for Carbon fusion ...
... "Planetary Nebulae" - Low mass star (< 8 Msun) cannot achieve 600 Million K temp. needed for Carbon fusion ...
CBradleyLoutl
... thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: - Age: . For a star around one solar mass, it takes a few million years to move to the main sequence. At twice this mass it takes less than a m ...
... thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: - Age: . For a star around one solar mass, it takes a few million years to move to the main sequence. At twice this mass it takes less than a m ...
Solution to Problem Set 1 1. The total number of nucleons in one
... the total energy received in a time period of t = 1s is E = f At = 9.6 × 10−15 J. The photons are mostly in the visible range, so have a wavelength λ ≈ 5500Å. Each photon has an energy of = hc/λ = 3.6 × 10−19 J, so the total number of photons is then E/ = 2.7 × 104 photons. 4. See the lecture no ...
... the total energy received in a time period of t = 1s is E = f At = 9.6 × 10−15 J. The photons are mostly in the visible range, so have a wavelength λ ≈ 5500Å. Each photon has an energy of = hc/λ = 3.6 × 10−19 J, so the total number of photons is then E/ = 2.7 × 104 photons. 4. See the lecture no ...
Stellar Evolution
... • If a protostar forms with a mass less than 0.08 solar masses, its internal temperature never reaches a value high enough for thermonuclear fusion to begin. • This failed star is called a brown dwarf, halfway between a planet (like Jupiter) and a star. ...
... • If a protostar forms with a mass less than 0.08 solar masses, its internal temperature never reaches a value high enough for thermonuclear fusion to begin. • This failed star is called a brown dwarf, halfway between a planet (like Jupiter) and a star. ...
IPHAS: Surveying the Northern Galactic Plane in Hα
... (red) stars in the (r'– i',r'–Hα) plane according to spectral type. The right-hand panel shows the observed sources in a field in the Cygnus region (black points), with some spectroscropically determined spectral types overplotted in colour; light blue points are early-type stars, red points are mos ...
... (red) stars in the (r'– i',r'–Hα) plane according to spectral type. The right-hand panel shows the observed sources in a field in the Cygnus region (black points), with some spectroscropically determined spectral types overplotted in colour; light blue points are early-type stars, red points are mos ...
Evolution of Massive Stars
... stars of lower initial mass. Like lower-mass stars, high-mass stars fuse hydrogen in their cores during their main sequence lifetime. Massive stars also spend 90% of the total lifetimes as stars located on the main sequence. The main sequence is also a time sequence – more massive stars complete the ...
... stars of lower initial mass. Like lower-mass stars, high-mass stars fuse hydrogen in their cores during their main sequence lifetime. Massive stars also spend 90% of the total lifetimes as stars located on the main sequence. The main sequence is also a time sequence – more massive stars complete the ...
N(M)
... These are the recombination lines and forbidden (also called collisionally excited) lines. Hydrogen and helium produce most recombination lines, whereas metals produce most forbidden lines in typical nebular conditions. ...
... These are the recombination lines and forbidden (also called collisionally excited) lines. Hydrogen and helium produce most recombination lines, whereas metals produce most forbidden lines in typical nebular conditions. ...
Stars - Red, Blue, Old, New pt.2
... • Leads us to the conclusion that mass is a very important factor in stellar evolution • The more massive a star is, the faster it will evolve (due to faster thermonuclear reaction rates in core) • Main sequence lifetime of sun is 12 billion years; 50xsun only about 50,000 years ...
... • Leads us to the conclusion that mass is a very important factor in stellar evolution • The more massive a star is, the faster it will evolve (due to faster thermonuclear reaction rates in core) • Main sequence lifetime of sun is 12 billion years; 50xsun only about 50,000 years ...
ASTRONOMY 157 – Stars and Galaxies - Syllabus
... calculation, Cepheid distances and exoplanet detection ...
... calculation, Cepheid distances and exoplanet detection ...
Ch. 11 and 12 Study Guide (ANSWERS)
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.