Asteroid 4 Vesta: Simultaneous visible and ultraviolet IUE observations☆
References (41)
- et al.
UBV photometry of Vesta
Icarus
(1979) - et al.
Ultraviolet reflectance properties of asteroids
Icarus
(1985) Ultraviolet observations of small bodies in the Solar System by OAO-2
Icarus
(1975)- et al.
Flattening, pole, and albedo features of 4 Vesta from photometric data
Icarus
(1987) - et al.
Surface properties of asteroids: A synthesis of polarimetry, radiometry, and spectrophotometry
Icarus
(1975) - et al.
Albedo and color contrasts on asteroid surfaces
Icarus
(1979) - et al.
Speckle interferometry of asteroids. IV. Reconstructed images of 4 Vesta
Icarus
(1988) Distribution of spin axes and senses of rotation for 20 large asteroids
Icarus
(1986)- et al.
Visible and near-infrared lightcurves of eight asteroids
Icarus
(1985) - et al.
Spectral geometric albedos of the Galilean satellites from 0.24–0.34 micron: Observations with the International Ultraviolet Observer Spacecraft
Icarus
(1987)
The rotation period and pole orientation of asteroid 4 Vesta
Icarus
Atlas of reflectance spectra of terrestrial, lunar, and meteoritic powders and frosts from 92 to 1800 nm
Icarus
FES sensitivity changes
IUE NASA Newslett.
Asteroids: The big picture
Magnitudes, colors, types and adopted diameters of the asteroids
Colorimetry and magnitudes of asteroids
Comparison of lunar ultraviolet reflectivity with that of terrestrial rocks samples
Moon
Revision of the absolute calibration of the LWP camera in low dispersion
IUE NASA Newslett.
Vesta's shape, density and albedo features
Astron. Astrophys.
Asteroid surface variegation
Cited by (9)
Olivine or impact melt: Nature of the "Orange" material on Vesta from Dawn
2013, IcarusCitation Excerpt :Vesta is the largest differentiated asteroid with a basaltic surface that is mostly intact today. Since 1929, Vesta’s surface has been extensively studied using ground-based telescopes in the ultraviolet, visible and infrared wavelength ranges (Bobrovnikoff, 1929; McFadden et al., 1977; Blanco and Catalano, 1979; Taylor et al., 1985; Festou et al., 1991; Gaffey, 1997; Hendrix et al., 2003; Zellner et al., 2005; Rivkin et al., 2006; Reddy et al., 2010) and using Hubble Space Telescope (HST) data (Thomas et al., 1997; Li et al., 2010, 2011). All these studies led to a better understanding of the mineralogy, space weathering effects and the global shape of Vesta.
Ultraviolet spectroscopy of Asteroid (4) Vesta
2011, IcarusCitation Excerpt :In orbit around it, Dawn will perform a detailed survey of its surface characteristics, internal structure, and elemental abundance targeted to understanding its formation and evolution (Russell et al., 2007). Rotationally resolved IUE observations showed single-peaked rotational lightcurves in the UV from 240 nm to 320 nm (Festou et al., 1991; Hendrix et al., 2003). The UV albedo of Vesta is less than 0.10, much lower than its visible albedo of ∼0.37 (Schevchenko and Tedesco, 2006).
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Partially based on IUE observations obtained at Villafranca del Castillo, Spain.
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Guest observer with the International Ultraviolet Explorer Observatory
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Permanent address; Observatoire Midi-Pyrénées, 14 avenue E. Belin, URA 285 du CNRS, F-31400 Toulouse, France