Using color photometry to separate transiting exoplanets from false
... same V −I as the constant component while being slightly bluer (the ∆(B − I)s shown is Fig. 2 are for the constant component) and moreover be at least moderately grazing. This is helpful, as grazing eclipses are swallower, requiring that that the separation between the two components must be reduced ...
... same V −I as the constant component while being slightly bluer (the ∆(B − I)s shown is Fig. 2 are for the constant component) and moreover be at least moderately grazing. This is helpful, as grazing eclipses are swallower, requiring that that the separation between the two components must be reduced ...
The Corn Burned by Syrius
... entropy considered below. The retention in the title of the variant, though historically legitimate, spelling of the star’s name – philologically associating it with an identifiable translation of the Consolation – acts as a consequential link to the classical model of divine stellar influence from ...
... entropy considered below. The retention in the title of the variant, though historically legitimate, spelling of the star’s name – philologically associating it with an identifiable translation of the Consolation – acts as a consequential link to the classical model of divine stellar influence from ...
Electronic Text Book Unit 11
... Days Earth’s axis is the imaginary line that passes through its center and connects the North and South poles. Earth’s spinning on its axis is called rotation (Figure 30.2) and it brings about day and night. If you have ever watched the sun travel during the day, you know that it appears to travel t ...
... Days Earth’s axis is the imaginary line that passes through its center and connects the North and South poles. Earth’s spinning on its axis is called rotation (Figure 30.2) and it brings about day and night. If you have ever watched the sun travel during the day, you know that it appears to travel t ...
A Digital Spectral Classification Atlas
... When the MK system was first defined, it was based on photographic spectra in the blue-violet part of the spectrum. This was done by necessity, as scientific photographic emulsions in the 1940’s were sensitive only to blue-violet light. However, it was a fortunate choice, as the blue-violet portion ...
... When the MK system was first defined, it was based on photographic spectra in the blue-violet part of the spectrum. This was done by necessity, as scientific photographic emulsions in the 1940’s were sensitive only to blue-violet light. However, it was a fortunate choice, as the blue-violet portion ...
Alpha Centauri
... Never viewed from northern latitudes(around 40 degrees) Traveling south below the earths surface, across the equator you will see it. ...
... Never viewed from northern latitudes(around 40 degrees) Traveling south below the earths surface, across the equator you will see it. ...
FOE 2017 Poster Contributions - College of Science | Oregon State
... core-collapse of a massive star or from the thermonuclear detonation of a white dwarf, is a central problem of modern astrophysics. For a handful of SNe, we have been able to identify the progenitor from pre-explosion images (e.g., Gerke et al., 2015; Adams et al., 2016); however, for supernova remn ...
... core-collapse of a massive star or from the thermonuclear detonation of a white dwarf, is a central problem of modern astrophysics. For a handful of SNe, we have been able to identify the progenitor from pre-explosion images (e.g., Gerke et al., 2015; Adams et al., 2016); however, for supernova remn ...
Stars: Intro & Classification Astronomy 1 — Elementary Astronomy LA Mission College
... LA Mission College Spring F2015 ...
... LA Mission College Spring F2015 ...
Mn, Cu, and Zn abundances in barium stars and their correlations
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
Abundances and possible diffusion of elements in M 67 stars⋆
... determinations T eff (V − Ks ) and T eff (V − Ic ) is 14 K ± 48 K (s.d). In Fig. 3 we have plotted the temperatures determined from Hα vs. the means of the two photometric temperatures with the correction mentioned above. It is seen that these two temperature scales agree well. The mean difference is − ...
... determinations T eff (V − Ks ) and T eff (V − Ic ) is 14 K ± 48 K (s.d). In Fig. 3 we have plotted the temperatures determined from Hα vs. the means of the two photometric temperatures with the correction mentioned above. It is seen that these two temperature scales agree well. The mean difference is − ...
A Bayesian method for the detection of planetary transits
... Of course, such a possibility only arises in the eventuality that the observer’s line of sight lies within the orbital plane of the planet. The probability for this to occur is, under the geometrical assumption, simply given by the star over planet radius ratio (0.0025 for the Sun-Jupiter system). T ...
... Of course, such a possibility only arises in the eventuality that the observer’s line of sight lies within the orbital plane of the planet. The probability for this to occur is, under the geometrical assumption, simply given by the star over planet radius ratio (0.0025 for the Sun-Jupiter system). T ...
Epsilon Aurigae: a rare stellar eclipse - Project VS
... geometrically thin, dark, dense, but partially transparent cloud can be seen passing in front of epsilon Aurigae. The images taken over a month clearly show the black silhouette of the disc beginning to move across the surface of the primary star. The size of the disc was measured at about 2.4 billi ...
... geometrically thin, dark, dense, but partially transparent cloud can be seen passing in front of epsilon Aurigae. The images taken over a month clearly show the black silhouette of the disc beginning to move across the surface of the primary star. The size of the disc was measured at about 2.4 billi ...
High-precision abundances of elements in solar twin stars: Trends
... Context. High-precision determinations of abundances of elements in the atmospheres of the Sun and solar twin stars indicate that the Sun has an unusual low ratio between refractory and volatile elements. This has led to the suggestion that the relation between abundance ratios, [X/Fe], and elementa ...
... Context. High-precision determinations of abundances of elements in the atmospheres of the Sun and solar twin stars indicate that the Sun has an unusual low ratio between refractory and volatile elements. This has led to the suggestion that the relation between abundance ratios, [X/Fe], and elementa ...
The major properties of the Interstellar Medium (ISM) are described
... • Observations of the velocities and distances of nearby stars and cepheid variables for distances of up to a few kpc from the sun - after which absorption and scattering extinguish light. • λ21cm, recombination line and CO radial velocity measurements of gas clouds in the ISM for distance greater t ...
... • Observations of the velocities and distances of nearby stars and cepheid variables for distances of up to a few kpc from the sun - after which absorption and scattering extinguish light. • λ21cm, recombination line and CO radial velocity measurements of gas clouds in the ISM for distance greater t ...
Binary mass ratios: system mass not primary mass
... We argue that to compare binaries one must examine the distributions of binary properties by system mass rather than by primary mass. If most binaries are primordial (as we argued above) then some physical process acts to fragment (or not) a system into two components and distributes the mass betwee ...
... We argue that to compare binaries one must examine the distributions of binary properties by system mass rather than by primary mass. If most binaries are primordial (as we argued above) then some physical process acts to fragment (or not) a system into two components and distributes the mass betwee ...
Practical cosmology with the Local Volume galaxies
... frame shows the local Hubble flow to be generally calm with peculiar velocity variations within ± 30 km/s. There is only a small area of negative peculiar velocities about - 250 km/s in direction towards the Leo constellation. According to Tully et al. (2008) this phenomena (the Local Velocity Anoma ...
... frame shows the local Hubble flow to be generally calm with peculiar velocity variations within ± 30 km/s. There is only a small area of negative peculiar velocities about - 250 km/s in direction towards the Leo constellation. According to Tully et al. (2008) this phenomena (the Local Velocity Anoma ...
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.