![NGC 6231: a young open cluster under X-rays](http://s1.studyres.com/store/data/008082437_1-7e7c74683a2b2b6d138973741b232724-300x300.png)
Galaxies - University of Iowa Astrophysics
... A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
... A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
on the pms star hbc 498 and its associated nebulous stars1
... trapezium of young stellar objects (Cohen 1980; Cohen & Kuhi 1979) associated with a small dark cloud in the direction of L1641(see Figure 1). The separation between any two stars in the trapezium is of about 0.20 pc (at a distance of 460 pc). The 25 year old spectrophotometric (resolution ∆λ = 7 Å ...
... trapezium of young stellar objects (Cohen 1980; Cohen & Kuhi 1979) associated with a small dark cloud in the direction of L1641(see Figure 1). The separation between any two stars in the trapezium is of about 0.20 pc (at a distance of 460 pc). The 25 year old spectrophotometric (resolution ∆λ = 7 Å ...
Do We Know of Any Maunder Minimum Stars?
... candidates are evolved or subgiant stars, not sunlike stars in a temporary state of very low activity. Figures 3 and 4 show the distribution of activity levels for stars in the WMBV and Mount Wilson catalogs. To derive ∆MV values for the Mount Wilson data, I applied the same methodology as in §3.1, ...
... candidates are evolved or subgiant stars, not sunlike stars in a temporary state of very low activity. Figures 3 and 4 show the distribution of activity levels for stars in the WMBV and Mount Wilson catalogs. To derive ∆MV values for the Mount Wilson data, I applied the same methodology as in §3.1, ...
Hot Horizontal Branch Stars in the Galactic Bulge. I
... (reviewed by Friel 1995), the most striking occurrence of sdB/O stars is found in NGC 6791, with a metallicity 3 – 4 times solar (Peterson & Green 1998). In addition to two cooler BHB (or blue straggler) members, the cluster harbors four or five sdB/O stars (Liebert, Saffer, & Green 1994) whose memb ...
... (reviewed by Friel 1995), the most striking occurrence of sdB/O stars is found in NGC 6791, with a metallicity 3 – 4 times solar (Peterson & Green 1998). In addition to two cooler BHB (or blue straggler) members, the cluster harbors four or five sdB/O stars (Liebert, Saffer, & Green 1994) whose memb ...
Meteor Shower Observations
... Most meteors are simply random bits of material orbiting the Sun that run into the Earth. These are called sporadic meteors. As the Earth goes around the Sun, more meteors hit the front of the Earth in it orbit, just as more bugs hit the front of a car driving down the highway. The front of the Eart ...
... Most meteors are simply random bits of material orbiting the Sun that run into the Earth. These are called sporadic meteors. As the Earth goes around the Sun, more meteors hit the front of the Earth in it orbit, just as more bugs hit the front of a car driving down the highway. The front of the Eart ...
SkyWatcher2017.5 1.3 Mb - Boise Astronomical Society
... twice this month from certain parts of the world. The Sun is located in Aries on May 1st. It enters Taurus on May 14th. In the evening, Mars is in the northeast and Jupiter in the southeast. Jupiter is located in the southwest and Saturn in the southeast at midnight. Mercury and Venus can be seen in ...
... twice this month from certain parts of the world. The Sun is located in Aries on May 1st. It enters Taurus on May 14th. In the evening, Mars is in the northeast and Jupiter in the southeast. Jupiter is located in the southwest and Saturn in the southeast at midnight. Mercury and Venus can be seen in ...
Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... stars often relied on spectra of rather low resolution and low S/N ratio, so that only limited information could be derived from the centroid wavelength of unresolved isotopic blends. In this paper we present the results of a study of the isotopic compositions of Hg and Pt in 5 very slowly rotating ...
... stars often relied on spectra of rather low resolution and low S/N ratio, so that only limited information could be derived from the centroid wavelength of unresolved isotopic blends. In this paper we present the results of a study of the isotopic compositions of Hg and Pt in 5 very slowly rotating ...
Sec 30.1 - Highland High School
... orbiting the center of the Milky Way, astronomers then used RR Lyrae variables to determine the distances to them. ...
... orbiting the center of the Milky Way, astronomers then used RR Lyrae variables to determine the distances to them. ...
THE N/O RATIO IN EARLY B-TYPE MAIN SEQUENCE STARS AS
... solar atmosphere. We note that the elemental abundances here and in the following are given in the standard logarithmic scale, where for hydrogen it is assumed that logH 12.00 . Since, according to Ref. 14, for temperatures Teff > 18500 K the derived abundance of C is low (by up to 0.2 dex) be ...
... solar atmosphere. We note that the elemental abundances here and in the following are given in the standard logarithmic scale, where for hydrogen it is assumed that logH 12.00 . Since, according to Ref. 14, for temperatures Teff > 18500 K the derived abundance of C is low (by up to 0.2 dex) be ...
POSTERS SESSION I: Atmospheres of Massive Stars
... We demonstrate that it is possible to have clumping occur close to the star while still achieving an excellent fit to Hα by consistently treating the wind’s rotation in the spectral modeling. An excellent agreement to other important optical lines such as HeII 4686 Å and NIII 4634–4640 Å is also o ...
... We demonstrate that it is possible to have clumping occur close to the star while still achieving an excellent fit to Hα by consistently treating the wind’s rotation in the spectral modeling. An excellent agreement to other important optical lines such as HeII 4686 Å and NIII 4634–4640 Å is also o ...
ALFALFA H-alpha: The Star-Formation-Rate Density
... Pluto, and more than four years to reach the nearest star, Proxima Centauri. For the measurement of SFR we have to deal with much greater times of travel and distances. Measurements of the historical SFRs have been taken up to a redshift of four (z = 4); this light has traveled for almost 12 billion ...
... Pluto, and more than four years to reach the nearest star, Proxima Centauri. For the measurement of SFR we have to deal with much greater times of travel and distances. Measurements of the historical SFRs have been taken up to a redshift of four (z = 4); this light has traveled for almost 12 billion ...
Sample pages 1 PDF
... the beginning of the twentieth century, things began to change. In 1934, the International Astronomical Union divided the sky into 88 constellations with precisely defined borders. Today we know exactly which constellation even the faintest star belongs to. For today’s astronomer, a constellation is ...
... the beginning of the twentieth century, things began to change. In 1934, the International Astronomical Union divided the sky into 88 constellations with precisely defined borders. Today we know exactly which constellation even the faintest star belongs to. For today’s astronomer, a constellation is ...
Wolf-Rayet Stars
... the star to velocities that exceed the surface escape speed. The observed spectrum originates over a range of radii with the optical continuum forming close to the stellar core, while the emission lines originate from a volume that can extend beyond 10 stellar radii. The observed mass-loss rates (i. ...
... the star to velocities that exceed the surface escape speed. The observed spectrum originates over a range of radii with the optical continuum forming close to the stellar core, while the emission lines originate from a volume that can extend beyond 10 stellar radii. The observed mass-loss rates (i. ...
12-1 - Piscataway High School
... one with another and decide which was emitting more light and which less. Of course, the stars are scattered at different distances, and you can’t shove them around to line them up for comparison. If, however, you know the distance to a star, you can use the inverse square relation to calculate the ...
... one with another and decide which was emitting more light and which less. Of course, the stars are scattered at different distances, and you can’t shove them around to line them up for comparison. If, however, you know the distance to a star, you can use the inverse square relation to calculate the ...
Metal-poor Stars
... for the number N of atoms of elements A and B, and refers to the Sun. With few exceptions, [Fe/H] traces the overall metallicity of the objects fairly well. To illustrate the difference between younger metal-rich and older metalpoor stars, Figure 1 shows spectra of the Sun and two of the most meta ...
... for the number N of atoms of elements A and B, and refers to the Sun. With few exceptions, [Fe/H] traces the overall metallicity of the objects fairly well. To illustrate the difference between younger metal-rich and older metalpoor stars, Figure 1 shows spectra of the Sun and two of the most meta ...
Astronomy 250 - University of Victoria
... Example: Suppose you are trying to measure the brightness of a star. You observe the star ten times, measure the brightness in each image, and find the average brightness from those 10 observations. However, you notice that the brightness changes slightly in each image, which means that your average ...
... Example: Suppose you are trying to measure the brightness of a star. You observe the star ten times, measure the brightness in each image, and find the average brightness from those 10 observations. However, you notice that the brightness changes slightly in each image, which means that your average ...
The Stars - Springer
... Ionized calcium (CaII), weak hydrogen CaII prominent, very weak hydrogen Neutral metals, faint hydrogen, hydrocarbon bands Molecular bands, titanium oxide (TiO) ...
... Ionized calcium (CaII), weak hydrogen CaII prominent, very weak hydrogen Neutral metals, faint hydrogen, hydrocarbon bands Molecular bands, titanium oxide (TiO) ...
Notes on Stars
... fundamental diagram of stellar astrophysics: the color-magnitude diagram or Hertzsprung-Russel diagram. Already around 1910, Rosenberg, Hertzsprung and Russel discuss what is now called the Hertsprung-Russel Diagram. The name Hertzsprung-Russel diagram is reserved for a diagram which shows luminosit ...
... fundamental diagram of stellar astrophysics: the color-magnitude diagram or Hertzsprung-Russel diagram. Already around 1910, Rosenberg, Hertzsprung and Russel discuss what is now called the Hertsprung-Russel Diagram. The name Hertzsprung-Russel diagram is reserved for a diagram which shows luminosit ...
The Starry Gnosis - Archidoxical Order of Magi
... In much of the Magick of the previous aeon, this emotionalism or ‘Bhakti’ is expressed through devotional, religious fervor; based on the sacred valuation of the godhead. Of course, the “awe and fear of the Creator” (Demiurge) is supplanted by the Holy Guardian Angel (Adonai) in Thelemic Magick. Yet ...
... In much of the Magick of the previous aeon, this emotionalism or ‘Bhakti’ is expressed through devotional, religious fervor; based on the sacred valuation of the godhead. Of course, the “awe and fear of the Creator” (Demiurge) is supplanted by the Holy Guardian Angel (Adonai) in Thelemic Magick. Yet ...
Chemical abundances and winds of massive stars in M31: a B
... types), Mg, Si, S, Al, Ca, Fe, Ti, Cr, Ni; Venn et al. 2000, Smartt, Dufton & Lennon 1997). Further they can also provide new information on the distances of galaxies through the detailed study of the strengths of their radiatively driven winds using the wind momentum – luminosity relationship (WLR, ...
... types), Mg, Si, S, Al, Ca, Fe, Ti, Cr, Ni; Venn et al. 2000, Smartt, Dufton & Lennon 1997). Further they can also provide new information on the distances of galaxies through the detailed study of the strengths of their radiatively driven winds using the wind momentum – luminosity relationship (WLR, ...
arXiv:astro-ph/0508448v1 22 Aug 2005
... massive enough to collapse to a black hole rather than a neutron star (Fryer 1999, van den Heuvel et al. 2000). The level of wind ...
... massive enough to collapse to a black hole rather than a neutron star (Fryer 1999, van den Heuvel et al. 2000). The level of wind ...
Supernovae - University of Texas Astronomy Home Page
... heavens favored Kepler in his turn with the explosion of a supernova in 1604. Kepler also took careful data by which we deduce that he witnessed the same kind of explosion as his master. Although there are counterarguments and some controversy, both Tycho's and Kepler's supernovae are widely regard ...
... heavens favored Kepler in his turn with the explosion of a supernova in 1604. Kepler also took careful data by which we deduce that he witnessed the same kind of explosion as his master. Although there are counterarguments and some controversy, both Tycho's and Kepler's supernovae are widely regard ...
preprint, pdf version - LESIA
... events observed in Brazil and Chile (4 June 2011) and in Hawaii (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of ...
... events observed in Brazil and Chile (4 June 2011) and in Hawaii (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of ...
Corona Australis
![](https://commons.wikimedia.org/wiki/Special:FilePath/Constellation_Corona_Australis.jpg?width=300)
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.