Discovery [1] | |
---|---|
Discovered by | B. Jekhovsky |
Discovery site | Algiers Obs. |
Discovery date | 27 March 1922 |
Designations | |
(976) Benjamina | |
Named after | Benjamin Jekhowsky Jr. (discoverer's son) [2] |
A922 FD · A910 AB 1922 LU · 1910 AB | |
main-belt
[1] · (
outer)
[3] background [4] [5] | |
Orbital characteristics [3] | |
Epoch 31 May 2020 ( JD 2459000.5) | |
Uncertainty parameter 0 | |
Observation arc | 109.34 yr (39,935 d) |
Aphelion | 3.5276 AU |
Perihelion | 2.8744 AU |
3.2010 AU | |
Eccentricity | 0.1020 |
5.73 yr (2,092 d) | |
43.757 ° | |
0° 10m 19.56s / day | |
Inclination | 7.7121° |
243.76° | |
319.60° | |
Physical characteristics | |
Mean diameter | |
9.701±0.002 h [9] [10] | |
Pole
ecliptic latitude | (354.0°, 80.0°) (λ1/β1) [5] [11] |
9.3 [1] [3] | |
976 Benjamina ( prov. designation: A922 FD or 1922 LU) is a dark background asteroid from the outer regions of the asteroid belt, approximately 81 kilometers (50 miles) in diameter. It was discovered on 27 March 1922, by Russian-French astronomer Benjamin Jekhowsky at the Algiers Observatory in North Africa. [1] The large X/ D-type asteroid has a rotation period of 9.7 hours and is likely regular in shape. It was named after the discoverer's son. [2]
Benjamina is a non- family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [4] [5] It orbits the Sun in the outer main-belt at a distance of 2.9–3.5 AU once every 5 years and 9 months (2,092 days; semi-major axis of 3.2 AU). Its orbit has an eccentricity of 0.10 and an inclination of 8 ° with respect to the ecliptic. [3]
The asteroid was first observed as A910 AB (1910 AB) at Heidelberg Observatory on 8 January 1910. The body's observation arc begins at the Crimean Simeiz Observatory in September 1930, more than 7 years after its official discovery observation at Algiers Observatory in March 1922. [1]
This minor planet was named after Benjamin Jekhowsky Jr., son of discoverer Benjamin Jekhowsky. The naming was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 93). [2]
In the Tholen classification, and based on a noisy spectra (:), Benjamina is an X-type asteroid, somewhat similar to that of a dark D-type (XD), which are common in the outer asteroid belt and among the Jupiter trojan population. [3]
In September 2004, a rotational lightcurve of Benjamina was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of 9.701±0.002 hours with a brightness variation of 0.19±0.01 magnitude ( U=3). Follow-up observation by his college René Roy in March 2018, determined a concurring period of 9.705±0.003 hours but with a much higher amplitude of 0.60±0.10 magnitude ( U=2). [9] [10] The objects first lightcurve was obtained by Colin Bembrick at Mount Tarana Observatory ( 431) in Australia in March 2003. It showed a period of 9.746±0.003 hours with an amplitude of 0.18±0.02 magnitude ( U=2). The overall amplitude suggest a rather regular shape with a ratio of 0.86 for the length of the a and b axes. [12]
In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia probe's second data release. It showed a sidereal period of 9.7080±0.0002 hours, and gave a spin axis at (354.0°, 80.0°) in ecliptic coordinates (λ, β). [5] [11]
According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Benjamina measures 79.94±1.16, 80.53±2.5 and 83.195±0.542 kilometers in diameter with an albedo of its surface of 0.057±0.002, 0.0559±0.004 and 0.052±0.006, respectively. [6] [7] [8] Additional measurements by the WISE telescope were published giving a mean-diameter as low as 71.372±27.828 km, and as high as 85.251±1.364 km. [5] [10]
The Collaborative Asteroid Lightcurve Link adopts the result from IRAS, that is, an albedo of 0.0559 and a diameter of 80.53 kilometers based on an absolute magnitude of 9.22. [10]
The asteroid had been observed in 7 stellar occultation events since 2003. [13] On 19 July 2003 the mag. 5.7 star HIP 88816 was occulted by the asteroid, [14] and was observed at 11 stations; 1 in Argentina, 3 in New Zealand, and 7 in Australia. From these observations, the best-fit ellipse measures 85.2 x 56.2 +/-12.4 kilometres.
Discovery [1] | |
---|---|
Discovered by | B. Jekhovsky |
Discovery site | Algiers Obs. |
Discovery date | 27 March 1922 |
Designations | |
(976) Benjamina | |
Named after | Benjamin Jekhowsky Jr. (discoverer's son) [2] |
A922 FD · A910 AB 1922 LU · 1910 AB | |
main-belt
[1] · (
outer)
[3] background [4] [5] | |
Orbital characteristics [3] | |
Epoch 31 May 2020 ( JD 2459000.5) | |
Uncertainty parameter 0 | |
Observation arc | 109.34 yr (39,935 d) |
Aphelion | 3.5276 AU |
Perihelion | 2.8744 AU |
3.2010 AU | |
Eccentricity | 0.1020 |
5.73 yr (2,092 d) | |
43.757 ° | |
0° 10m 19.56s / day | |
Inclination | 7.7121° |
243.76° | |
319.60° | |
Physical characteristics | |
Mean diameter | |
9.701±0.002 h [9] [10] | |
Pole
ecliptic latitude | (354.0°, 80.0°) (λ1/β1) [5] [11] |
9.3 [1] [3] | |
976 Benjamina ( prov. designation: A922 FD or 1922 LU) is a dark background asteroid from the outer regions of the asteroid belt, approximately 81 kilometers (50 miles) in diameter. It was discovered on 27 March 1922, by Russian-French astronomer Benjamin Jekhowsky at the Algiers Observatory in North Africa. [1] The large X/ D-type asteroid has a rotation period of 9.7 hours and is likely regular in shape. It was named after the discoverer's son. [2]
Benjamina is a non- family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [4] [5] It orbits the Sun in the outer main-belt at a distance of 2.9–3.5 AU once every 5 years and 9 months (2,092 days; semi-major axis of 3.2 AU). Its orbit has an eccentricity of 0.10 and an inclination of 8 ° with respect to the ecliptic. [3]
The asteroid was first observed as A910 AB (1910 AB) at Heidelberg Observatory on 8 January 1910. The body's observation arc begins at the Crimean Simeiz Observatory in September 1930, more than 7 years after its official discovery observation at Algiers Observatory in March 1922. [1]
This minor planet was named after Benjamin Jekhowsky Jr., son of discoverer Benjamin Jekhowsky. The naming was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 93). [2]
In the Tholen classification, and based on a noisy spectra (:), Benjamina is an X-type asteroid, somewhat similar to that of a dark D-type (XD), which are common in the outer asteroid belt and among the Jupiter trojan population. [3]
In September 2004, a rotational lightcurve of Benjamina was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of 9.701±0.002 hours with a brightness variation of 0.19±0.01 magnitude ( U=3). Follow-up observation by his college René Roy in March 2018, determined a concurring period of 9.705±0.003 hours but with a much higher amplitude of 0.60±0.10 magnitude ( U=2). [9] [10] The objects first lightcurve was obtained by Colin Bembrick at Mount Tarana Observatory ( 431) in Australia in March 2003. It showed a period of 9.746±0.003 hours with an amplitude of 0.18±0.02 magnitude ( U=2). The overall amplitude suggest a rather regular shape with a ratio of 0.86 for the length of the a and b axes. [12]
In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia probe's second data release. It showed a sidereal period of 9.7080±0.0002 hours, and gave a spin axis at (354.0°, 80.0°) in ecliptic coordinates (λ, β). [5] [11]
According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Benjamina measures 79.94±1.16, 80.53±2.5 and 83.195±0.542 kilometers in diameter with an albedo of its surface of 0.057±0.002, 0.0559±0.004 and 0.052±0.006, respectively. [6] [7] [8] Additional measurements by the WISE telescope were published giving a mean-diameter as low as 71.372±27.828 km, and as high as 85.251±1.364 km. [5] [10]
The Collaborative Asteroid Lightcurve Link adopts the result from IRAS, that is, an albedo of 0.0559 and a diameter of 80.53 kilometers based on an absolute magnitude of 9.22. [10]
The asteroid had been observed in 7 stellar occultation events since 2003. [13] On 19 July 2003 the mag. 5.7 star HIP 88816 was occulted by the asteroid, [14] and was observed at 11 stations; 1 in Argentina, 3 in New Zealand, and 7 in Australia. From these observations, the best-fit ellipse measures 85.2 x 56.2 +/-12.4 kilometres.