Chapter 21 notes - Clinton Public Schools
... galaxy instead. Lots of dust and gas. Universe: All of space and everything in it. Numbers astronomers use are either very small or very large: scientific notation is useful in astronomy Section 5: The Expanding Universe: How the universe was formed: Astronomers believe the universe was incredibly h ...
... galaxy instead. Lots of dust and gas. Universe: All of space and everything in it. Numbers astronomers use are either very small or very large: scientific notation is useful in astronomy Section 5: The Expanding Universe: How the universe was formed: Astronomers believe the universe was incredibly h ...
Galaxies - Indiana University Astronomy
... Using the same website as above, click on “spectrum” for the two galaxies whose distances you measured. The optical spectrum of the galaxy is shown at the top of the spectrum page. Shown are many different spectral features, including absorption lines and emission lines, superimposed on continuum em ...
... Using the same website as above, click on “spectrum” for the two galaxies whose distances you measured. The optical spectrum of the galaxy is shown at the top of the spectrum page. Shown are many different spectral features, including absorption lines and emission lines, superimposed on continuum em ...
Properties of Ellipticals and Spirals
... The central regions are somewhat redder, while the spiral arms are bluer. The Spiral Arms get fainter and fainter and extend FAR out. ...
... The central regions are somewhat redder, while the spiral arms are bluer. The Spiral Arms get fainter and fainter and extend FAR out. ...
Lecture 13
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
5X_Measuring_galaxy_redshifts
... wavelength’, such that the Doppler shift is the same for all channels. Largescale variations are then filtered out (i.e. only spectral lines left). The spectrum is then ‘slid’ against a template prepared from a known bright galaxy or star, and a correlation function derived. The peaks in the functio ...
... wavelength’, such that the Doppler shift is the same for all channels. Largescale variations are then filtered out (i.e. only spectral lines left). The spectrum is then ‘slid’ against a template prepared from a known bright galaxy or star, and a correlation function derived. The peaks in the functio ...
Astronomy Quiz 12 “Stars
... A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is called __ motion. A. radial B. proper C. real D. transverse _____4. How far away ...
... A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is called __ motion. A. radial B. proper C. real D. transverse _____4. How far away ...
Stellar evolution, II
... As the hydrogen in the core of a star is transformed into helium, the matter in the core becomes degenerate. In a low density gas many possible energy levels of the electrons are open, but as the gas become denser all the lower energy levels are filled. The Pauli exclusion principle states that eac ...
... As the hydrogen in the core of a star is transformed into helium, the matter in the core becomes degenerate. In a low density gas many possible energy levels of the electrons are open, but as the gas become denser all the lower energy levels are filled. The Pauli exclusion principle states that eac ...
Eyeing the retina nebula
... Planetary nebulae play a key role in recycling these materials throughout the universe. Without them rocky planets like the Earth and carbon-based life forms like us would not exist. The image of the Retina Nebula has been enhanced to dramatize its beauty. The difference in brightness between the ce ...
... Planetary nebulae play a key role in recycling these materials throughout the universe. Without them rocky planets like the Earth and carbon-based life forms like us would not exist. The image of the Retina Nebula has been enhanced to dramatize its beauty. The difference in brightness between the ce ...
Orion- The Swordsman of the Sky - A Winter Constellation from the
... however does require a telescope to see it. The Orion Nebula also holds fainter objects, which require magnification to see them, such as the Horse Head Nebula. You have to imagine, and possibly take your finger to join the dots, but you can virtually see the shoulders of Orion. The left shoulder s ...
... however does require a telescope to see it. The Orion Nebula also holds fainter objects, which require magnification to see them, such as the Horse Head Nebula. You have to imagine, and possibly take your finger to join the dots, but you can virtually see the shoulders of Orion. The left shoulder s ...
Colour - Magnitude Diagram for M 45
... The Pleiades is a relatively close open cluster. The six or seven stars visible to the naked eye form a tight grouping of stars (an asterism) near the even closer Hyades cluster. They are easily visible in the winter sky in the northern hemisphere. In this exercise, you will determine the colour of ...
... The Pleiades is a relatively close open cluster. The six or seven stars visible to the naked eye form a tight grouping of stars (an asterism) near the even closer Hyades cluster. They are easily visible in the winter sky in the northern hemisphere. In this exercise, you will determine the colour of ...
Death of massive stars
... Supernova Explosions of Massive Stars • As a star develops an iron core, energy production declines, and the core contracts. –Nuclear reactions involving iron begin. –However, they remove energy from the core—causing it to contract even further. –Once this process starts, the core of the star colla ...
... Supernova Explosions of Massive Stars • As a star develops an iron core, energy production declines, and the core contracts. –Nuclear reactions involving iron begin. –However, they remove energy from the core—causing it to contract even further. –Once this process starts, the core of the star colla ...
earth & space science
... Scientists estimate that over a period of almost 5 billion years, the sun has converted only 5% of its original hydrogen nuclei into helium nuclei. ...
... Scientists estimate that over a period of almost 5 billion years, the sun has converted only 5% of its original hydrogen nuclei into helium nuclei. ...
Thought Question
... B. It would be -3 magnitudes brighter C. It would stay the same (its absolute magnitude is an intrinsic property of a star) ...
... B. It would be -3 magnitudes brighter C. It would stay the same (its absolute magnitude is an intrinsic property of a star) ...
Astro 10 Practice Test 2
... d. Mostly iron, similar to the hot iron core of the Earth, with a little bit of helium and some heavier elements. 17. On a clear autumn night, you spend some time examining the glowing HII regions in the galaxy M33, using a large reflecting telescope. If you were IN the galaxy M33, looking at these ...
... d. Mostly iron, similar to the hot iron core of the Earth, with a little bit of helium and some heavier elements. 17. On a clear autumn night, you spend some time examining the glowing HII regions in the galaxy M33, using a large reflecting telescope. If you were IN the galaxy M33, looking at these ...
Quasars - Ann Arbor Earth Science
... Seyfert galaxy - luminous, star-like nuclei with strong emission lines. On closer inspection it is a galaxy, usually a spiral or disturbed system, whose strong emission lines are too broad and of ionization too high to be produced by the galaxy's stellar population. In type 1 Seyferts, some of the ...
... Seyfert galaxy - luminous, star-like nuclei with strong emission lines. On closer inspection it is a galaxy, usually a spiral or disturbed system, whose strong emission lines are too broad and of ionization too high to be produced by the galaxy's stellar population. In type 1 Seyferts, some of the ...
A small mass difference between Hydrogen and Helium The
... From periodic wobbling back and forth of the spectral lines of a (blended) binary, we can often determine the radius of the orbit, and orbital speeds, and thus the masses of the stars From observations of binaries, we have the masses Of a sample of stars, and can study how stellar Properties depend ...
... From periodic wobbling back and forth of the spectral lines of a (blended) binary, we can often determine the radius of the orbit, and orbital speeds, and thus the masses of the stars From observations of binaries, we have the masses Of a sample of stars, and can study how stellar Properties depend ...
The power plant of the Sun and stars
... October 1, 0:39 AM October 3, 9:28 PM October 6, 6:17 PM Also check eclipsing binary Beta Lyrae, P=12.939412 days ...
... October 1, 0:39 AM October 3, 9:28 PM October 6, 6:17 PM Also check eclipsing binary Beta Lyrae, P=12.939412 days ...
lecture25
... We find mostly hot, massive stars in the spiral arms of galaxies because 1) hot, massive stars are preferentially produced in the spiral arms 2) less massive stars live long enough to rotate out of the spiral arms 3) supernovae destroy the less massive stars in the spiral arms 4) there is too high a ...
... We find mostly hot, massive stars in the spiral arms of galaxies because 1) hot, massive stars are preferentially produced in the spiral arms 2) less massive stars live long enough to rotate out of the spiral arms 3) supernovae destroy the less massive stars in the spiral arms 4) there is too high a ...
Chapter 19 Star Formation
... globular clusters are that the globular clusters are very old, while the open clusters are much younger. The absence of massive Main Sequence stars in the globular cluster is due to its extreme age—those stars have already used up their fuel and have moved off the Main Sequence. ...
... globular clusters are that the globular clusters are very old, while the open clusters are much younger. The absence of massive Main Sequence stars in the globular cluster is due to its extreme age—those stars have already used up their fuel and have moved off the Main Sequence. ...
10 September: Faint Stars and Bright Stars
... Absolute Magnitude: a measure of the intrinsic brilliance of a star • Pick a star (any star) • Imagine moving it to a distance of 10 parsecs • The apparent magnitude it would have is its absolute magnitude • The absolute magnitude is a distanceindependent quantity • Look at Appendix 12 and Appendix ...
... Absolute Magnitude: a measure of the intrinsic brilliance of a star • Pick a star (any star) • Imagine moving it to a distance of 10 parsecs • The apparent magnitude it would have is its absolute magnitude • The absolute magnitude is a distanceindependent quantity • Look at Appendix 12 and Appendix ...
Chapter 19 Star Formation
... globular clusters are that the globular clusters are very old, while the open clusters are much younger. The absence of massive Main Sequence stars in the globular cluster is due to its extreme age—those stars have already used up their fuel and have moved off the Main Sequence. ...
... globular clusters are that the globular clusters are very old, while the open clusters are much younger. The absence of massive Main Sequence stars in the globular cluster is due to its extreme age—those stars have already used up their fuel and have moved off the Main Sequence. ...
Bright stars and faint stars: the stellar magnitude system Magnitudes
... • Imagine moving it to a distance of 10 parsecs • The apparent magnitude it would have is its absolute magnitude • The absolute magnitude is a distanceindependent quantity • Look at Appendix 12 and Appendix 13 (the brightest stars) and think about the meaning of the absolute magnitudes ...
... • Imagine moving it to a distance of 10 parsecs • The apparent magnitude it would have is its absolute magnitude • The absolute magnitude is a distanceindependent quantity • Look at Appendix 12 and Appendix 13 (the brightest stars) and think about the meaning of the absolute magnitudes ...
LESSON 4, STARS
... becomes a protostar, a main-sequence star, a red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a ...
... becomes a protostar, a main-sequence star, a red giant, and finally, a white dwarf. A more-massive star: begins as a nebula, becomes a protostar, a main-sequence star, a very massive star, a supergiant, a supernova, and finally, either a neutron star (pulsar) or a ...
Lesson 4, Stars
... Objectives Define some of the properties of stars. Compare the evolutionary paths of star ...
... Objectives Define some of the properties of stars. Compare the evolutionary paths of star ...
Space Science Distance Definitions
... means of measuring the luminosity of a star should find the same value. However, apparent brightness is not an intrinsic property of the star; it depends on your location. • Why do light sources appear fainter as a function of distance? The reason is that as light travels towards you, it is spreadin ...
... means of measuring the luminosity of a star should find the same value. However, apparent brightness is not an intrinsic property of the star; it depends on your location. • Why do light sources appear fainter as a function of distance? The reason is that as light travels towards you, it is spreadin ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.