1604 Tombaugh
| Discovery | |
|---|---|
| Discovered by | C. O. Lampland |
| Discovery site | Lowell Obs. |
| Discovery date | 24 March 1931 |
| Designations | |
| MPC designation | 1604 Tombaugh |
|
Named after
|
Clyde Tombaugh (astronomer) |
| 1931 FH · 1930 DX 1933 SA1 · 1936 FA 1937 JH · 1941 CF 1943 OE · 1948 ME 1949 ST1 · A920 EC |
|
| main-belt · Eos | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 96.43 yr (35,221 days) |
| Aphelion | 3.3296 AU |
| Perihelion | 2.7161 AU |
| 3.0229 AU | |
| Eccentricity | 0.1015 |
| 5.26 yr (1,920 days) | |
| 321.85° | |
| 0° 11m 15s / day | |
| Inclination | 9.3951° |
| 309.10° | |
| 38.244° | |
| Physical characteristics | |
| Dimensions |
28.78±0.53 km 32.25 km (derived) 32.33±2.2 km (IRAS:3) |
|
6.15 h (dated) 7.04 h (dated) 7.047±0.004 h 7.056±0.001 h 8.2 h (dated) |
|
| 0.0933 (derived) 0.1038±0.016 (IRAS:3) 0.138±0.006 |
|
|
B–V = 0.751 U–B = 0.373 XSCU (Tholen) · Xc (SMASS) · X |
|
| 10.4 · 10.53 · 10.65 · 10.93±0.15 | |
1604 Tombaugh, provisional designation 1931 FH, is a rare-type Eoan asteroid from the outer region of the asteroid belt, approximately 32 kilometers in diameter. It was discovered on 24 March 1931, by American astronomer Carl Otto Lampland at Lowell Observatory in Flagstaff, Arizona, in the United States.
Tombaugh is a member of the Eos family. It is classified as a X-type asteroid, as well as a rare XSCU and intermediate Xc type in the Tholen and SMASS taxonomy, respectively. It orbits the Sun at a distance of 2.7–3.3 AU once every 5 years and 3 months (1,920 days). Its orbit has an eccentricity of 0.10 and an inclination of 9° with respect to the ecliptic. Previously identified as A920 EC and 1930 DX at Heidelberg in 1920 and 1930, Tombaugh's observation arc begins one year prior to its official 1931-discovery at Flagstaff.
In April 2010 and November 2012, two rotational light-curves of Tombaugh were obtained from photometric observations at Oakley Southern Sky Observatory, Australia, and at Bassano Bresciano Observatory, Italy, respectively. The light-curve analysis gave a rotation period of 7.047 and 7.056 hours with a brightness variation of 0.16 and 0.35 magnitude, respectively (U=2+/2+), These periods supersede previous results obtained by astronomers Claes-Ingvar Lagerkvist (1975), Richard P. Binzel (1984) and Krisztián Sárneczky (U=1/2/2).
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