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• W76836788 abstract "The Near-Earth Asteroid (NEA) 4055 Magellan was discovered by Glo Helin at Palomar Mountain (IAUC 4638) and was one of the first known minor planets with surface reflectance properties comparable to that of 4 Vesta (Tholen, 1988). Broadband photometry and near-IR spectroscopy revealed strong 0.9 and 1.9 micron proxene bands, suggesting a compositional similarity of 4055 Magellan with that of 4 Vesta and the basaltic achondrite meteorites (Cruikshank et al. 1991). In anticipation of the Dawn mission to 4 Vesta we obtained 5 partial nights of Bessel R photometry of 4055 Magellan at the Jet Propulsion Laboratory Table Mountain Observatory 0.6-m telescope (TMO). We measured a synodic period of 7.488+/-0.001 hr, similar to the 7.475+-0.001 hr period obtained by Pravec et al. (www.asu.cas.cz/~ppravec/newres.txt). Our object exhibited a large lightcurve amplitude (∆M~0.8 mag) implying a highly elongated shape. We used our TMO photometry and the Absolute Magnitude as tabulated by the Minor Planet Center to construct a rudimentary solar phase curve. We derived a phase parameter g = 0.30, similar to the phase behavior as measured by Pravec and colleagues (www.asu.cas.cz/~ppravec/neo.html). Our high g implies a shallow solar phase slope, consistent with the object's high albedo (ρ = 0.31) obtained from thermal measurements (Delbo et al. 2003). The photometric properties of the V-type 4055 Magellan, such as shallow phase slope and high albedo, are consistent with 4 Vesta, giving us confidence in using NEA vestoids as photometric analogs for 4 Vesta. Methods: Our goal was to construct a lightcurve for 4055 Magellan giving us insight about its physical characteristics. The observed magnitudes were extracted from photometry collected over a span of 5 nights at TMO (2010 August 9/10/12/13/14). Using the H-G magnitude system (Bowell et al, 1989), Reduced Magnitudes were calculated by V(α) = Vobs (α) – 5logr∆ where r is the heliocentric distance, ∆ the geocentric distance, both in AU, and α is the solar phase angle. Absolute magnitudes, H, were obtained from equation (Bowell et al, 1989) H(α) = H – 2.5log[(1 G)φ1(α) + Gφ2(α)] where H, is the Reduced Magnitude at mean brightness and at solar phase angle 0°. G is the slope parameter. It is scaled in a manner such that G ≈ 0 for low albedo bodies and G > 0.25 for high albedo bodies (Bowell et al,1989). φ1(α) and φ2(α) are specified phase functions given by equation φi = exp[-Ai(tan0.5α) i] ; i = 1, 2 A1 = 3.33 A2 = 1.87 B1 = 0.63 B2 = 1.22 Our photometric data was superimposed to generate a composite lightcurve with a complete rotational phase. The key to constructing an accurate lightcurve was determining 4055 Magellan's synodic period. In order to do so, for each test period used, rotational phase values, ψ, were calculated. Rotational phase was found by ψi,k = ( tk– t0 ) / pi i,k = 1, 2,... where pi is the test period, tk is the time stamp of an exposure in units of Julian Days and t0 is the data point chosen to be the zero value. Rotational phase was calculated for the time stamp of each exposure. These values were calculated for each test period." @default.
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• W76836788 date "2011-05-01" @default.
• W76836788 modified "2023-09-24" @default.
• W76836788 title "Rotationally Resolved Photometry of the V-type Near-Earth Asteroid 4055 Magellan (1985 DO2)" @default.
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