958 Asplinda (prov. designation: or ) is a resonant Hilda asteroid, approximately in diameter, located in the outermost region of the asteroid belt. It was discovered on 28 September 1921, by astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The assumed C-type asteroid has a rotation period of 16.5 hours and is likely elongated in shape. It was named after Swedish astronomer Bror Asplind (1890–1954). Orbit and classification Asplinda is a member of the distant orbital Hilda group of asteroids, which stay in a 3:2 orbital resonance with Jupiter. It is however not a member of the collisional Hilda family () but a non-family asteroid of the background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outermost asteroid belt at a distance of 3.2–4.7 AU once every 7 years and 11 months (2,905 days; semi-major axis of 3.98 AU). Its orbit has an eccentricity of 0.18 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins at Heidelberg on 24 October 1921, four weeks after its official discovery observation. Naming This minor planet was named after Bror Ansgar Asplind (1890–1954), a Swedish astronomer and orbit computer. The following, sequentially numbered asteroids 959 Arne, 960 Birgit and 961 Gunnie are named after his three children, respectively. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics No spectral type has been published for Asplinda. As an Hildian asteroid with a low albedo (see below) it is a carbonaceous C-type asteroid (assumed), or possibly a D-type or P-type asteroid, which are very common among the Hildian and more distant Jupiter trojan population. Rotation period and poles In December 2017, a rotational lightcurve of Asplinda was obtained from photometric observations by Brian Warner, Robert Stephens and Daniel Coley at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of hours with a high brightness amplitude of magnitude, indicative of an elongated, non-spherical shape (). The results supersedes previous observations with a period determination of by the same astronomers in 2016, and a period of published by Mats Dahlgren in 1998 (). The 2017 observations by Warner, Stephens and Coley also gave two spin axes of (228.0°, 33.0°) and (46.0°, 45.0°) in ecliptic coordinates (λ, β) and a sidereal period of hours. These results