in Allen''''s Astrophysical Quantities

By J. Drilling, A. Landolt. 2000

1,424 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Optical and Infrared Photometry of the Nearby Type Ia Supernova 2001el (2002, background): “We note that the optical and infrared colors of this star are entirely consistent with it being a normal K2 III star (Allen & Cox 2000).”
Spitzer Reveals Hidden Quasar Nuclei in Some Powerful FR II Radio Galaxies (2006, neutral): “For Galactic-type dust, A(7, 15, 35 µm)/A(V) = (0.020, 0.015, 0.004) (Mathis 2000).”
The distances to Galactic low-mass X-ray binaries: consequences for black hole luminosities and kicks (2004, methodology): “For a K0V/III star the (V K)0 colour is 1.96/2.31 ( Cox 2000 ), using the relations between the (V K)0 colour and the surface brightness as determined by Bailey (1981) we get a lower limit to the distance of 2.7 kpc for a K0III and 3 kpc for a K0V companion star (again we used R2 = 6 ± 1R⊙ after Sha”
Physics of Solar Prominences: I—Spectral Diagnostics and Non-LTE Modelling (2010, background): “The photo-ionization cross-section is inversely proportional to some power of the photon frequency (Keady and Kilcrease 2000; Anzer and Heinzel 2005); a plot of the average cross-section per atom/ion for an assumed prominence composition is provided in Fig.”
Variable Infrared Emission from the Supermassive Black Hole at the Center of the Milky Way (2003, methodology): “In our 2002 map, the new L’ source is blended with the star S0-2, which at this time was experiencing its closest approach to the SMBH with a projected separation of a mere 14 mas 2003a,b).”
NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 (2016, positive): “Along with it, IAU 2015 Resolution B2 adopted the de ﬁ nition of the parsec to be exactly 648,000 / π au ( Binney & Tremaine 2008; see also Cox 2000 ) .”
CESAM: a free code for stellar evolution calculations (2008, methodology): “Iben & MacDonald (1985), Cox et al. (1989), Thoul et al.”
Accurate fundamental parameters for 23 bright solar-type stars (2010, methodology): “For four others,α For, γ Ser,β Aql and δ Pav, onlyνmax has been measured. However, Kjeldsen & Bedding (1995) determined a scal ing between∆ν andνmax as”
THE SOLAR NEIGHBORHOOD. XXXVII. THE MASS–LUMINOSITY RELATION FOR MAIN-SEQUENCE M DWARFS (2016, background): “The dashed line is the locus of dwarf (luminosity class V) stars of various spectral types; the dot-dashed line is for giants (luminosity class III) from Cox (2000). The reddening vector indicates AV = 1.”
ON THE USE OF EMPIRICAL BOLOMETRIC CORRECTIONS FOR STARS (2010, methodology): “REFERENCES Allen, C. W. 1976, Astrophysical Quantities, 3rd Ed.”
GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, neutral): “…with isotropic energy release > 4×1046 erg. Refs: [1] Guetta & Della Valle 2007; [2] Soderberg et al. 2006; [3a] Nakar, Gal-Yam & Fox 2006; [3b] Coward et al. 2012; [4] Kalogera et al. 2004; [5] Ofek 2007; [6] Scannapieco & Bildsten 2005; [7] Li et al. 2011 [8] Lorimer et al. 2007; [9]…”
Stellar Processes Near the Massive Black Hole in the Galactic Center (2005, background): “An approximate association of mass with spectral type is indicated in the upper horizontal axis (Cox 2000).”