The Milky Way
... The only way to explain the rotation curve of our galaxy is to say that there is lots and lots of mass that is not emitting light. The halo of our galaxy must be full of it. The halo outweighs the disk by a factor of 10. As far as we can tell, this mass doesn’t emit any ...
... The only way to explain the rotation curve of our galaxy is to say that there is lots and lots of mass that is not emitting light. The halo of our galaxy must be full of it. The halo outweighs the disk by a factor of 10. As far as we can tell, this mass doesn’t emit any ...
Understanding the Astrophysics of Galaxy Evolution: the role of
... question has suffered because the emission lines needed to diagnose the presence of an AGN (Hα and [NII]λ6548) are already redshifted into the near-IR part of the spectrum at z ∼ 1, and hence are inaccessible with current instruments. ...
... question has suffered because the emission lines needed to diagnose the presence of an AGN (Hα and [NII]λ6548) are already redshifted into the near-IR part of the spectrum at z ∼ 1, and hence are inaccessible with current instruments. ...
Populations of Galaxies and their Formation at z < 7
... How many stars are there in the universe? Integrated mass function at z = 0: Integrated history z = 0 - 1000 ...
... How many stars are there in the universe? Integrated mass function at z = 0: Integrated history z = 0 - 1000 ...
Unit 1
... • Low-mass protostars become stars very slowly – Weaker gravity causes them to contract slowly, so they heat up gradually – Weaker gravity requires low-mass stars to compress their cores more to get hot enough for fusion – Low-mass stars have higher density! ...
... • Low-mass protostars become stars very slowly – Weaker gravity causes them to contract slowly, so they heat up gradually – Weaker gravity requires low-mass stars to compress their cores more to get hot enough for fusion – Low-mass stars have higher density! ...
talk.wyse - Johns Hopkins University
... ΛCDM cosmology extremely successful on large scales. Galaxies are the scales on which one must see the nature of dark matter & galaxy formation astrophysics Ostriker & Steinhardt 03 ...
... ΛCDM cosmology extremely successful on large scales. Galaxies are the scales on which one must see the nature of dark matter & galaxy formation astrophysics Ostriker & Steinhardt 03 ...
Chapter 1 Introduction
... Lying behind much of the work in this thesis are the predictions from a pillar of modern astronomy, the theory of stellar evolution. e changes in the structure of a star over its lifetime are now very well understood, and they are largely determined by a single parameter: its mass. Although the Sun ...
... Lying behind much of the work in this thesis are the predictions from a pillar of modern astronomy, the theory of stellar evolution. e changes in the structure of a star over its lifetime are now very well understood, and they are largely determined by a single parameter: its mass. Although the Sun ...
printer-friendly version of benchmark
... For mid-mass stars, such as our Sun, this is called the red giant stage, where helium is being fused into carbon. Scientists have gathered strong evidence that our Sun will become, in about 5 billion years, a red giant where its outer layer may spread as wide as Earth’s orbit. The temperature of our ...
... For mid-mass stars, such as our Sun, this is called the red giant stage, where helium is being fused into carbon. Scientists have gathered strong evidence that our Sun will become, in about 5 billion years, a red giant where its outer layer may spread as wide as Earth’s orbit. The temperature of our ...
Exam 2
... example, some of the heavy elements (such as carbon, nitrogen and oxygen) that form in a star’s core move into its outer layers. The abundance of these elements in a planetary nebula can show how material mixes through the various parts of a star’s interior. The expanding nebula merges with the inte ...
... example, some of the heavy elements (such as carbon, nitrogen and oxygen) that form in a star’s core move into its outer layers. The abundance of these elements in a planetary nebula can show how material mixes through the various parts of a star’s interior. The expanding nebula merges with the inte ...
3D Tour of the Universe Template
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
Chapter 14
... • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once the period is measured, the luminosity is known and we can proceed as above. ...
... • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once the period is measured, the luminosity is known and we can proceed as above. ...
Millisecond Pulsar Binaries at Transition
... can switch between the states of having an accretion disk and being disk-free in a short time scale of 10 years They are likely at the transition phase from LMXBs to MSP binaries, during which interesting multi-wavelength properties are displayed Other possibility is they could be at the state o ...
... can switch between the states of having an accretion disk and being disk-free in a short time scale of 10 years They are likely at the transition phase from LMXBs to MSP binaries, during which interesting multi-wavelength properties are displayed Other possibility is they could be at the state o ...
スライド 1 - STScI
... Figure 2 is the I-K vs. K color-magnitude diagram of variable stars in the LMC. Relevant data is taken from Ita et al. (2004). The horizontal line shows the 10 sigma detection limit for our monitoring survey at K band, which is about 15.5 magnitude. The right diagonal line stands for the 10 sigma de ...
... Figure 2 is the I-K vs. K color-magnitude diagram of variable stars in the LMC. Relevant data is taken from Ita et al. (2004). The horizontal line shows the 10 sigma detection limit for our monitoring survey at K band, which is about 15.5 magnitude. The right diagonal line stands for the 10 sigma de ...
Navigating the Night Sky – Teacher Guide Argos Online Subject
... • Download and print the two star wheels: Basic Constellations Star Wheel & Coordinates Star Wheel 3. Get star maps for concurrent (ideally the two most recent) months. These can be found in Stardate Magazine, or online at Skymaps.com http://www.skymaps.com/downloads.html - go to middle of webpage a ...
... • Download and print the two star wheels: Basic Constellations Star Wheel & Coordinates Star Wheel 3. Get star maps for concurrent (ideally the two most recent) months. These can be found in Stardate Magazine, or online at Skymaps.com http://www.skymaps.com/downloads.html - go to middle of webpage a ...
Lecture 9: The interstellar medium (ISM)
... than the surrounding medium (normally HI) and they therefore expand supersonically (~ 10 km/s) into the surrounding gas. ...
... than the surrounding medium (normally HI) and they therefore expand supersonically (~ 10 km/s) into the surrounding gas. ...
m V
... the line of sight • Colour is blue, as blue light is the most readily scattered • Scattering of light from blue stars, usually type B; spectrum is also of this type, i.e. absorption lines • Light is often highly polarized (20 – 30 per cent) • Amongst best known examples are the reflection nebulae fr ...
... the line of sight • Colour is blue, as blue light is the most readily scattered • Scattering of light from blue stars, usually type B; spectrum is also of this type, i.e. absorption lines • Light is often highly polarized (20 – 30 per cent) • Amongst best known examples are the reflection nebulae fr ...
... • Some galaxies are spiral like the Milky Way while others are egg-shaped or completely irregular in appearance • Besides shape, galaxies vary greatly in the star, gas, and dust content and some are more “active” than others • Galaxies tend to cluster together and these clusters appear to be separat ...
Galaxies
... • Astronomers now have decided that the morphology classification should consist of only two types of galaxies: the spiral and the elliptical. • Barred spirals are a subclass of spirals. Irregulars may be either spiral or barred spiral. ...
... • Astronomers now have decided that the morphology classification should consist of only two types of galaxies: the spiral and the elliptical. • Barred spirals are a subclass of spirals. Irregulars may be either spiral or barred spiral. ...
Finish up Sun and begin Stars of the Sun Test 1 Study
... • Important as determines actual brightness but hard to measure as stars are so far away Closest Alpha Centauri 4.3 light years = 4 x 1013 km (1 AU = distance Earth to Sun = 8 light minutes) • Close stars use stellar parallax (heliocentric parallax or triangulation same meaning) • Can “easily” mea ...
... • Important as determines actual brightness but hard to measure as stars are so far away Closest Alpha Centauri 4.3 light years = 4 x 1013 km (1 AU = distance Earth to Sun = 8 light minutes) • Close stars use stellar parallax (heliocentric parallax or triangulation same meaning) • Can “easily” mea ...
Exploration of the Milky Way and Nearby galaxies
... To observe diffusion in action is to compare the elemental abundances for heavy elements near the Fe-peak of MS versus red giant and sub-giant stars in metalpoor globular clusters ...
... To observe diffusion in action is to compare the elemental abundances for heavy elements near the Fe-peak of MS versus red giant and sub-giant stars in metalpoor globular clusters ...
ASTR1102-002 Potentially useful facts and mathematical relations
... parallax of 0.15 arcsec/yr. Which star is moving through space with the faster speed? a. Star “A” is moving faster than star “B”. b. Star “B” is moving faster than star “A”. c. The stars are moving through space at the same speed. d. None of the above. (Briefly explain.) ANS: ...
... parallax of 0.15 arcsec/yr. Which star is moving through space with the faster speed? a. Star “A” is moving faster than star “B”. b. Star “B” is moving faster than star “A”. c. The stars are moving through space at the same speed. d. None of the above. (Briefly explain.) ANS: ...
- IRSF: Past and Future
... In this talk, I first describe how the cicumstellar interaction occurs in massive X-ray and gammaray binaries, using the results from 3D SPH simulations. Then, assuming that the NIR emission from the circumstellar material is due to the free-free emission, and using the simulated distribution of den ...
... In this talk, I first describe how the cicumstellar interaction occurs in massive X-ray and gammaray binaries, using the results from 3D SPH simulations. Then, assuming that the NIR emission from the circumstellar material is due to the free-free emission, and using the simulated distribution of den ...
Project 3. Colour in Astronomy
... where Fx is the observed flux in the band x, and Fvega is the flux of the star Vega. The star Vega, in the constellation of Lyra is used as a reference in the magnitude system. Vega has the arbitrary definition of zero magnitude at all wavelengths U=B=V=R=I=0 This does not mean tha ...
... where Fx is the observed flux in the band x, and Fvega is the flux of the star Vega. The star Vega, in the constellation of Lyra is used as a reference in the magnitude system. Vega has the arbitrary definition of zero magnitude at all wavelengths U=B=V=R=I=0 This does not mean tha ...
Red Giants - Faculty Web Pages
... Most blue stars are Main Sequence stars. But whereas some red stars in the list are simply tiny, cool Main Sequence stars, other red stars of the exact same color are huge Red Giants! Telling the difference between the Main Sequence red stars and the Red Giant stars involves some complex measurement ...
... Most blue stars are Main Sequence stars. But whereas some red stars in the list are simply tiny, cool Main Sequence stars, other red stars of the exact same color are huge Red Giants! Telling the difference between the Main Sequence red stars and the Red Giant stars involves some complex measurement ...
February 2013 - astronomy for beginners
... brightest stars are called Pollux (β) and Castor (α) and are known as the Gemini Twins. The twins originated in a Greek myth which told that they had one mother but two fathers. Castor was the mortal son of King Tyndareus but Pollux was the immortal son of the God Zeus who had disguised himself as C ...
... brightest stars are called Pollux (β) and Castor (α) and are known as the Gemini Twins. The twins originated in a Greek myth which told that they had one mother but two fathers. Castor was the mortal son of King Tyndareus but Pollux was the immortal son of the God Zeus who had disguised himself as C ...
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.