1370 Hella
Discovery[1]
Discovered byK. Reinmuth
Discovery siteHeidelberg Obs.
Discovery date31 August 1935
Designations
(1370) Hella
Named after
Helene Nowacki[2]
(ARI-astronomer)
1935 QG
main-belt · (inner)
Flora[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc81.46 yr (29,754 days)
Aphelion2.6343 AU
Perihelion1.8665 AU
2.2504 AU
Eccentricity0.1706
3.38 yr (1,233 days)
130.52°
0° 17m 31.2s / day
Inclination4.8039°
306.04°
3.9960°
Physical characteristics
Dimensions5.41 km (calculated)[3]
7.5408 h[5]
inconclusive[3]
0.24 (assumed)[3]
S (assumed)[3]
13.5[1][3] · 13.69±0.63[6]

    1370 Hella, provisional designation 1935 QG, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 5.4 kilometers in diameter. It was discovered on 31 August 1935, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany.[7] The asteroid was named for Helene Nowacki, an astronomer at the Astronomical Calculation Institute.[2]

    Orbit and classification

    Hella is a member of the Flora family (402),[3][4] a giant asteroid family and the largest family of stony asteroids in the main belt.[8]: 23 

    It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.6 AU once every 3 years and 5 months (1,233 days). Its orbit has an eccentricity of 0.17 and an inclination of 5° with respect to the ecliptic.[1] The body's observation arc begins at Heidelberg in September 1935, one month after its official discovery observation.[7]

    Physical characteristics

    According to its classification as a Florian asteroid, Hella is an assumed stony S-type asteroid.[3]

    Rotation period

    In October 2006, a rotational lightcurve of Hella was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave an inconclusive rotation period of 7.5408 hours with a brightness amplitude of 0.17 magnitude (U=n.a.).[5] The Lightcurve Data Base, however, only lists the measured brightness variation. As of 2017, no secure period of Hella has been obtained.[3]

    Diameter and albedo

    Hella has not been observed by any of the space-based surveys, such as the Infrared Astronomical Satellite (IRAS), the Japanese Akari satellite or the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora the parent body of the Flora Family – and calculates a diameter of 5.41 kilometers based on an absolute magnitude of 13.5.[3]

    Naming

    This minor planet was named after Helene Nowacki (1904–1972), a German astronomer of the Astronomical Calculation Institute. The name was suggested by astronomer Gustav Stracke. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 124).[2]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1370 Hella (1935 QG)" (2017-02-15 last obs.). Jet Propulsion Laboratory. Retrieved 31 October 2017.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1370) Hella". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 111. doi:10.1007/978-3-540-29925-7_1371. ISBN 978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 8 9 10 "LCDB Data for (1370) Hella". Asteroid Lightcurve Database (LCDB). Retrieved 31 October 2017.
    4. 1 2 "Asteroid 1370 Hella – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    5. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1370) Hella". Geneva Observatory. Retrieved 31 October 2017.
    6. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 31 October 2017.
    7. 1 2 "1370 Hella (1935 QG)". Minor Planet Center. Retrieved 31 October 2017.
    8. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
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