T. Kwiatkowski

CCD photometry and model of MUSES-C target (25143) 1998 SF36

We present photometric observations of the near-Earth asteroidxa0(25143) 1998xa0SF36 from the 2001xa0apparition campaign, and we discuss the corresponding physical model. The asteroids photometric behaviour is consistent with an S-type object, it has a retrograde pole at

Photometry of 2006 RH120: an asteroid temporary captured into a geocentric orbit

lambda=355^circ, beta=-84^circpm 5^circ

Photometry and models of selected main belt asteroids I. 52 Europa, 115 Thyra, and 382 Dodona

, and its sidereal rotation period is

Eclipsing binary asteroid 90 Antiope

P=12.132pm 0.0005

Photometric survey of the very small near-Earth asteroids with the SALT telescope - I. Lightcurves and periods for 14 objects

hours. 1998xa0SF36 is elongated, with rough global dimension ratiosxa0

New binary asteroid 809 Lundia - I. Photometry and modelling

a/b=2.0

Photometry and models of selected main belt asteroids. III. 283 Emma, 665 Sabine, and 690 Wratislavia

,

Eclipsing events in the binary system of the asteroid 90 Antiope

b/c=1.3

Photometry and models of selected main belt asteroids IV. 184 Dejopeja, 276 Adelheid, 556 Phyllis

, but the elongation is not due to a bifurcated shape. The surface is not likely to contain major concavities. No significant albedo variegation was detected.

Photometry and models of selected main belt asteroids - II. 173 Ino, 376 Geometria, and 451 Patientia

Aims. From July 2006 to July 2007 a very small asteroid orbited the Earth within its Hill sphere. We used this opportunity to study its rotation and estimate its diameter and shape. Methods. Due to its faintness, 2006 RH120 was observed photometrically with the new 10-m SALT telescope at the SAAO (South Africa). We obtained data on four nights: 11, 15, 16, and 17 March 2007 when the solar phase angle remained almost constant at 74 ◦ . The observations lasted about an hour each night and the object was exposed for 7−10 s through the “clear” filter. Results. From the lightcurves obtained on three nights we derived two solutions for a synodical period of rotation: P1 = 1.375 ± 0.001 min and P2 = 2.750 ± 0.002 min. The available data are not sufficient to choose between them. The absolute magnitude of the object was found to be H = 29.9 ± 0.3 mag (with the assumed slope parameter G = 0.25) and its effective diameter D = 2− 7m , depending on the geometric albedo pV (with the most typical near-Earth asteroids albedo pV = 0.18 its diameter would be D = 3.3 ± 0.4 m). The body has an elongated shape with the a/b ratio greater than 1.4. It probably originates in low-eccentricity Amor or Apollo orbits. There is still a possibility, which needs further investigation, that it is a typical near-Earth asteroid that survived the aerobraking in the Earth’s atmosphere and returned to a heliocentric orbit similar to that of the Earth.