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1 Discovery of peculiar periodic spectral
... the Fourier continuum as discussed in section 2. We could therefore have assumed that all the detections are due to the effect of noise; however if this were the case the detections would be uniformly distributed, within reasonable statistical fluctuation boundaries, as a function of the sampling nu ...
... the Fourier continuum as discussed in section 2. We could therefore have assumed that all the detections are due to the effect of noise; however if this were the case the detections would be uniformly distributed, within reasonable statistical fluctuation boundaries, as a function of the sampling nu ...
Astro Review - Parkway C-2
... 54. Describe what is happening to the star shown in Figure 25-2. 55. What type of star is shown in Figure 25-2? 56. What happens to a low-mass star when it depletes its hydrogen fuel? 57. Why do massive stars age faster than stars that are less massive? 58. Why does a red giant have a reddish appea ...
... 54. Describe what is happening to the star shown in Figure 25-2. 55. What type of star is shown in Figure 25-2? 56. What happens to a low-mass star when it depletes its hydrogen fuel? 57. Why do massive stars age faster than stars that are less massive? 58. Why does a red giant have a reddish appea ...
114EQ-AR
... These lines are known as Right Ascension and Declination. The celestial map also contains two poles and an equator just like a map of the Earth. The celestial poles are defined as those two points where the Earth's North and South poles, if extended to infinity, would cross the celestial sphere. Thu ...
... These lines are known as Right Ascension and Declination. The celestial map also contains two poles and an equator just like a map of the Earth. The celestial poles are defined as those two points where the Earth's North and South poles, if extended to infinity, would cross the celestial sphere. Thu ...
The spectroscopic Hertzsprung-Russell diagram
... the absolute brightnesses, i.e. the distances, are required to properly order the stars in the HR diagram. Also for stars in star clusters, where the distance may still be unknown, but the distances of all stars are roughly equal, order can be achieved in what we now call color-magnitude diagrams, s ...
... the absolute brightnesses, i.e. the distances, are required to properly order the stars in the HR diagram. Also for stars in star clusters, where the distance may still be unknown, but the distances of all stars are roughly equal, order can be achieved in what we now call color-magnitude diagrams, s ...
Book Describing Techniques to Detect Transiting ExoPlanets
... How things change! We now know that planets are everywhere in the galaxy. Billions upon billions of planets must exist! This is the message from the tally of ~ 400 extra-solar planetary systems (as of mid-2009). Among them are 60 exoplanets that transit in front of their star (46 that are brighter t ...
... How things change! We now know that planets are everywhere in the galaxy. Billions upon billions of planets must exist! This is the message from the tally of ~ 400 extra-solar planetary systems (as of mid-2009). Among them are 60 exoplanets that transit in front of their star (46 that are brighter t ...
The Evolution of Isotope Ratios in the Milky Way Galaxy
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
Angular Momentum Evolution of Young Low
... the best way to trace their angular momentum evolution from about 1 million years ago (Ma) to 1 billion years ago (Ga). This section discusses the observational studies of stellar rotation performed since the PPV review by Herbst al. (2007), for solar-type stars and lower-mass stars, down to the bro ...
... the best way to trace their angular momentum evolution from about 1 million years ago (Ma) to 1 billion years ago (Ga). This section discusses the observational studies of stellar rotation performed since the PPV review by Herbst al. (2007), for solar-type stars and lower-mass stars, down to the bro ...
Diapositiva 1
... The error depend on the Γ angle (0.5 μas accuracy) Parallactic displacement along the great cicle Sun-Star Sensitivity AL is proportional to sin ξ sin Γ ξ = Sun-spin axis angle = 45º for Gaia Γ = basic angle = 106.5º for Gaia Optimal values between astrometry requirements - that call for a large ang ...
... The error depend on the Γ angle (0.5 μas accuracy) Parallactic displacement along the great cicle Sun-Star Sensitivity AL is proportional to sin ξ sin Γ ξ = Sun-spin axis angle = 45º for Gaia Γ = basic angle = 106.5º for Gaia Optimal values between astrometry requirements - that call for a large ang ...
Multiwavelength observations of XTE J1118+480`s outburst
... 30% of sources detected by INTEGRAL/IBIS were not known. 80% of Norma sources are X-ray pulsars, high spin periods Spectra typical of neutron stars No radio emission 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local ...
... 30% of sources detected by INTEGRAL/IBIS were not known. 80% of Norma sources are X-ray pulsars, high spin periods Spectra typical of neutron stars No radio emission 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local ...
A catalogue of the Chandra Deep Field South with multi
... introduce artificial colour offsets and changing observing conditions are typical for ground-based observations, we need a non-standard photometry approach to measure spectral shapes accurately. In fact, we need to measure the same central fraction of an object in every band as it would appear in eq ...
... introduce artificial colour offsets and changing observing conditions are typical for ground-based observations, we need a non-standard photometry approach to measure spectral shapes accurately. In fact, we need to measure the same central fraction of an object in every band as it would appear in eq ...
Dynamical properties of a large young disk galaxy at z=2.03⋆
... Obviously, the first and foremost question that needs to be resolved is whether these objects are truly rotationally supported disks, and this can only be tested by obtaining kinematic data. In this paper, we present SINFONI observations of one of the large disks of the Labbé et al. sample (id 257 ...
... Obviously, the first and foremost question that needs to be resolved is whether these objects are truly rotationally supported disks, and this can only be tested by obtaining kinematic data. In this paper, we present SINFONI observations of one of the large disks of the Labbé et al. sample (id 257 ...
A Spitzer mid-infrared spectral survey of mass
... variability. Where further data are available, we list JHKL photometry averaged over the cycle in Table 2. Also listed are pulsation periods, taken from Whitelock et al. (2003), Wood (1998), Nishida et al. (2000), Ita et al. (2004) and Groenewegen (2004). Where available, periods from Whitelock et a ...
... variability. Where further data are available, we list JHKL photometry averaged over the cycle in Table 2. Also listed are pulsation periods, taken from Whitelock et al. (2003), Wood (1998), Nishida et al. (2000), Ita et al. (2004) and Groenewegen (2004). Where available, periods from Whitelock et a ...
Spring 2015 Mercury - Astronomical Society of the Pacific
... on the spot where the battle would take place and viciously attacked each other, thus predicting the violence that was to come. After the comet swung behind the Sun and reappeared on its journey An Anglo-Saxon penny with a portrait of to the outer solar system, it was King Cnut the Great and, possib ...
... on the spot where the battle would take place and viciously attacked each other, thus predicting the violence that was to come. After the comet swung behind the Sun and reappeared on its journey An Anglo-Saxon penny with a portrait of to the outer solar system, it was King Cnut the Great and, possib ...
Determination of accurate stellar radial
... ELODIE (Baranne et al. 1996) is an échelle spectrometer physically located in a coudé room at the 1.93 m telescope at Observatoire de Haute-Provence (OHP). For this programme, the spectrometer was fed via one optical fibre from the Cassegrain focus. The instrument FWHM is '7.2 km s−1 , correspondi ...
... ELODIE (Baranne et al. 1996) is an échelle spectrometer physically located in a coudé room at the 1.93 m telescope at Observatoire de Haute-Provence (OHP). For this programme, the spectrometer was fed via one optical fibre from the Cassegrain focus. The instrument FWHM is '7.2 km s−1 , correspondi ...
But Still, It Moves: Tides, Stellar Parallax, and Galileo`s
... occur, and that the time of day at which tides occur varies slowly over the course of a year as the Earth revolves around the Sun instead of over the course of a month as the Moon revolves around the Earth. Neither Johannes Kepler (1571-1630) nor René Descartes (1596-1650), two other prominent Coper ...
... occur, and that the time of day at which tides occur varies slowly over the course of a year as the Earth revolves around the Sun instead of over the course of a month as the Moon revolves around the Earth. Neither Johannes Kepler (1571-1630) nor René Descartes (1596-1650), two other prominent Coper ...
Correcting Systematic Poalrization Effects in Keck LRISp
... 1994; Johns-Krull & Valenti 1996, 2000) . We use them here as stars where we expect relatively large and detectable signals. The star HD20630 is a G5Vv star of BY Dra type. Though this star is magnetic with known variability, it is listed as a bright unpolarized standard star (in continuum filters) ...
... 1994; Johns-Krull & Valenti 1996, 2000) . We use them here as stars where we expect relatively large and detectable signals. The star HD20630 is a G5Vv star of BY Dra type. Though this star is magnetic with known variability, it is listed as a bright unpolarized standard star (in continuum filters) ...
Deneb - Emmi
... Deneb, which means tail in Arabic, is the 19th brightest star in the universe, and one of the most well known stars in our very own Milky Way. ...
... Deneb, which means tail in Arabic, is the 19th brightest star in the universe, and one of the most well known stars in our very own Milky Way. ...
Ch. 20 - Astro1010
... about the Galactic Center comes from observations at gamma ray, hard X-ray, ...
... about the Galactic Center comes from observations at gamma ray, hard X-ray, ...
Ursa Minor
![](https://en.wikipedia.org/wiki/Special:FilePath/Sidney_Hall_-_Urania's_Mirror_-_Draco_and_Ursa_Minor.jpg?width=300)
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.