Starwalk Manual En
... Spotter function will be activated. Star Walk™ uses the digital compass to learn which way you are looking. A live representation of what you see in the sky will appear on your display and the sky will start following your movements whether you move up or down, left or right. To turn off this functi ...
... Spotter function will be activated. Star Walk™ uses the digital compass to learn which way you are looking. A live representation of what you see in the sky will appear on your display and the sky will start following your movements whether you move up or down, left or right. To turn off this functi ...
Life on Other Worlds
... may throw them away upon such subjects as this; but I suppose they who can spend their time better, will not be at so vain and fruitless an expence." (John Glanvill's translation of 1688.) The question whether life exists on other worlds is one that still excites curiosity, and to which astronomers ...
... may throw them away upon such subjects as this; but I suppose they who can spend their time better, will not be at so vain and fruitless an expence." (John Glanvill's translation of 1688.) The question whether life exists on other worlds is one that still excites curiosity, and to which astronomers ...
Do We Know of Any Maunder Minimum Stars?
... a star with [Fe/H] = +0.3 will lie ∼ 0.45 magnitude above the main sequence of a solar-metallicity star, and a star with [Fe/H] = −0.3 will lie ∼ 0.45 magnitude beneath it. Stars evolve very slowly while they are on the main sequence, so ∆MV changes very little until a star begins to evolve toward t ...
... a star with [Fe/H] = +0.3 will lie ∼ 0.45 magnitude above the main sequence of a solar-metallicity star, and a star with [Fe/H] = −0.3 will lie ∼ 0.45 magnitude beneath it. Stars evolve very slowly while they are on the main sequence, so ∆MV changes very little until a star begins to evolve toward t ...
Neutron Stars
... electrons are not in the lowest-energy level near the nucleus; instead they are arranged in higher-energy-level shells. ...
... electrons are not in the lowest-energy level near the nucleus; instead they are arranged in higher-energy-level shells. ...
Navigation: The Mariner`s Quadrant
... (or elevation) between the horizon and Polaris. South of the equator, where the North Star is not visible, mariners would use the constellation known as the Southern Cross to determine their southern latitude. Located almost directly above the South Pole, the Southern Cross also never sets. Followin ...
... (or elevation) between the horizon and Polaris. South of the equator, where the North Star is not visible, mariners would use the constellation known as the Southern Cross to determine their southern latitude. Located almost directly above the South Pole, the Southern Cross also never sets. Followin ...
The ISO–SWS Spectrum of Planetary Nebula NGC 7027
... molecular hydrogen lines (H2 ) have been measured as well and probably originate in the outer part of the nebula where the temperature is lowest. For Ar, K and specially Ne we have information for the most important stages of ionization implying that the uncertainty in the ionization correction fact ...
... molecular hydrogen lines (H2 ) have been measured as well and probably originate in the outer part of the nebula where the temperature is lowest. For Ar, K and specially Ne we have information for the most important stages of ionization implying that the uncertainty in the ionization correction fact ...
Star formation rates from young-star counts and the structure of the
... et al. 2009; Heiderman et al. 2010; Lada, Lombardi & Alves 2010; Wu et al. 2010; Gutermuth et al. 2011). These studies have consistently shown that when one considers the immediate dense environment (on a few parsec scales) surrounding the newly formed stars, the derived SFR is higher than predicted ...
... et al. 2009; Heiderman et al. 2010; Lada, Lombardi & Alves 2010; Wu et al. 2010; Gutermuth et al. 2011). These studies have consistently shown that when one considers the immediate dense environment (on a few parsec scales) surrounding the newly formed stars, the derived SFR is higher than predicted ...
implication on the mass and
... color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
... color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
W. M. White Geochemistry Chapter 10: Cosmochemistry
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
... we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. The old stars of Population II are considerably poorer in heavy elements than are young stars. In particular, Population II stars have a Fe/H ratio typically a fa ...
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 ...
CORONAL EVOLUTION OF THE SUN IN TIME: HIGH
... coronal radio and X-ray emissions. The coronal emissions display the largest range of variation in response to the surface magnetic activity level. Whereas starspots may cover a few percent of the photosphere of the most active solar analogs, thus producing a photometric wave with a modulation depth ...
... coronal radio and X-ray emissions. The coronal emissions display the largest range of variation in response to the surface magnetic activity level. Whereas starspots may cover a few percent of the photosphere of the most active solar analogs, thus producing a photometric wave with a modulation depth ...
Long-term monitoring of the short period SU UMa
... here lasted about 2 weeks, suggesting that these superoutbursts belong to the intermediate category, or V844 4.1. superhump period change Her simply lies in the majority of SU UMa-type dwarf Historically, the superhump period had been known to novae. decrease during the course of the superoutburst b ...
... here lasted about 2 weeks, suggesting that these superoutbursts belong to the intermediate category, or V844 4.1. superhump period change Her simply lies in the majority of SU UMa-type dwarf Historically, the superhump period had been known to novae. decrease during the course of the superoutburst b ...
Neutron Star and Superfluidity
... The idea of superfluidity exists inside neutron stars was first proposed by Migdal[1]. In analogy to electrons inside superconductor forming cooper pairs due to electron lattice interaction, it is expected that nucleons in neutron star at sufficiently high density and low temperature can also form coppe ...
... The idea of superfluidity exists inside neutron stars was first proposed by Migdal[1]. In analogy to electrons inside superconductor forming cooper pairs due to electron lattice interaction, it is expected that nucleons in neutron star at sufficiently high density and low temperature can also form coppe ...
Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absorption column, smeared and probably delayed variability of fluorescent Fe line • Source is also interesting from the point of view of unusually high Lopt/ ...
... • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absorption column, smeared and probably delayed variability of fluorescent Fe line • Source is also interesting from the point of view of unusually high Lopt/ ...
Course Outline - Tony Bacigalupo
... has moved off the main sequence The star is internally unstable Cepheid variables are high mass stars RR Lyrae are low mass stars that hit the bottom edge of the strip ...
... has moved off the main sequence The star is internally unstable Cepheid variables are high mass stars RR Lyrae are low mass stars that hit the bottom edge of the strip ...
Habitable Zone Lifetimes of Exoplanets around Main Sequence Stars
... surface, experiencing high rates of evaporation and increasing humidity. The resulting increase in temperature serves to further accelerate evaporation, eventually resulting in the irreversible evaporation of the ocean into the atmosphere (Kasting, 1988; Goldblatt and Watson, 2012). The outer bounda ...
... surface, experiencing high rates of evaporation and increasing humidity. The resulting increase in temperature serves to further accelerate evaporation, eventually resulting in the irreversible evaporation of the ocean into the atmosphere (Kasting, 1988; Goldblatt and Watson, 2012). The outer bounda ...
Discovery of White Dwarfs—1 Oct • Adams’ discovery
... Apparent & Absolute Magnitude • Apparent mag is a logarithmetic expression of flux • If the apparent mag changes by −2.5, the flux is brighter by a factor of 10. • Fluxes and magnitudes of two stars A and B ...
... Apparent & Absolute Magnitude • Apparent mag is a logarithmetic expression of flux • If the apparent mag changes by −2.5, the flux is brighter by a factor of 10. • Fluxes and magnitudes of two stars A and B ...
A History of Star Catalogues - The Albuquerque Astronomical Society
... Hevelius was not pleased with his initial results. Luckily the city of Danzig gave him an azimuthal quadrant, two meters in radius, that had belonged to Krüger. He built several more instruments, but was not happy with their accuracy until he designed a nine foot radius sextant. Altogether he had mo ...
... Hevelius was not pleased with his initial results. Luckily the city of Danzig gave him an azimuthal quadrant, two meters in radius, that had belonged to Krüger. He built several more instruments, but was not happy with their accuracy until he designed a nine foot radius sextant. Altogether he had mo ...
A Detailed Derivation of the Radial Velocity Equation
... or the DOPPLER METHOD). The purpose of this paper is to derive the theoretical equation that is associated with the variation over time of a star’s velocity along an observer’s line‐of‐sight – a quantity that can be precisely measured with an optical telesco ...
... or the DOPPLER METHOD). The purpose of this paper is to derive the theoretical equation that is associated with the variation over time of a star’s velocity along an observer’s line‐of‐sight – a quantity that can be precisely measured with an optical telesco ...
Astronomy 140 Lecture Notes, Spring 2008 c
... along with program objects, in order to convert an observed flux ratio into a magnitude difference, which when combined with the known standard star magnitude gives the measured magnitude of the program object. The standard fluxes are usually given in erg/cm2 /sec/Hz for Fν or W/cm2 /sec/µm for Fλ , ...
... along with program objects, in order to convert an observed flux ratio into a magnitude difference, which when combined with the known standard star magnitude gives the measured magnitude of the program object. The standard fluxes are usually given in erg/cm2 /sec/Hz for Fν or W/cm2 /sec/µm for Fλ , ...
Celestial Navigation Second Edition
... at the data and help you learn what went wrong. Part of the learning process is exactly that. Leaning the pitfalls of possible mistakes and how to avoid them. This course offers so many practice examples, that you will have this under control before you set off. It is obviously much better to make a ...
... at the data and help you learn what went wrong. Part of the learning process is exactly that. Leaning the pitfalls of possible mistakes and how to avoid them. This course offers so many practice examples, that you will have this under control before you set off. It is obviously much better to make a ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.