Physical properties of PHA 2014 JO25 from a worldwide observational campaign

Aznar, Amadeo; León, J. de; Popescu, M.; Serra-Ricart, M.; Short, P.; Pravec, Petr; Văduvescu, O.; Licandro, J.; Ortiz, J. L.; Sota, A.; Morales, N.; Lorenzi, V.; Warner, Brian D.; Oey, Julian; Groom, R.

doi:10.1093/mnras/sty3250

Cited by 3 publications

(4 citation statements)

References 13 publications

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“…Our band parameters generally match or are close to previously published results, with some exceptions (Thomas et al 2014;Dunn et al 2013;Popescu et al 2014;Reddy et al 2022;Aznar et al 2019;Ieva et al 2015;Leith et al 2017). Ganymed's BAR varies in previously published data, causing it to often plot in the S(IV) region, in addition to the S(VI) region (Thomas et al 2014).…”

Section: Prism Bandssupporting

confidence: 91%

“…We will investigate potential spatial variability on Ganymed, as well as on Eros and Florence, in an upcoming paper. Our calculated BAR values for Heracles, 2002 QF15, and 2014 JO25 are generally higher than previously published values (e.g., Thomas et al 2014;Popescu et al 2014;Dunn et al 2013;Aznar et al 2019), significantly so for the latter two objects.…”

Section: Prism Bandscontrasting

confidence: 85%

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3 μm Spectroscopic Survey of Near-Earth Asteroids

et al. 2022

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Near-Earth Asteroids (NEAs) are excellent laboratories for processes that affect airless body surfaces. S-complex (including V-type) NEAs were not expected to contain OH/H2O on their surfaces because they formed in the anhydrous regions of the solar system and their surface temperatures are high enough to remove these volatiles. However, a 3 μm feature typically indicative of OH/H2O was identified on other seemingly dry bodies in the inner solar system, raising the question of how widespread volatiles may be on NEAs. We observed 29 NEAs using both prism (0.7–2.52 μm) and LXD_short (1.67–4.2 μm) modes on SpeX on NASA’s IRTF in order to accurately characterize asteroid spectral type and the 3 μm region. Eight of the observed NEAs have a 3 μm absorption feature at >1σ (three of which are present to >2σ), and they exhibit four identified band shape types. Possible sources for OH/H2O on these bodies include carbonaceous chondrite impacts and/or interactions with protons implanted by solar wind. Characteristics such as composition and aphelion appear to play an important role in the delivery and/or retention of OH/H2O, as all eight NEAs with an absorption feature are S-complex asteroids and six enter the main asteroid belt. Additionally, perihelion, size, albedo, and orbital period may play a minor role. Our observations determined that nominally anhydrous, inner solar system bodies, and therefore near-Earth space in general, contain more OH/H2O than previously expected. The identified trends should help predict which NEAs that have not yet been observed might contain OH/H2O on their surfaces.

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Section: Prism Bandssupporting

confidence: 91%

Section: Prism Bandscontrasting

confidence: 85%

3 μm Spectroscopic Survey of Near-Earth Asteroids

et al. 2022

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“…Brozovic et al (2017) have obtained a period of 4.5 hrs, whereas Warner (2017) has claimed three possible periods (3, 4.5 and 6 hours) for the asteroid. This rotation period of 4.5 hrs has also been confirmed by Aznar et al (2018) and Tan et al (2018). Aznar et al (2018) have used an extensive data set of 4540 data points to derive the rotation period.…”

Section: The Light Curvesupporting

confidence: 82%

“…This rotation period of 4.5 hrs has also been confirmed by Aznar et al (2018) and Tan et al (2018). Aznar et al (2018) have used an extensive data set of 4540 data points to derive the rotation period. However, all of these observations have been made starting from 20th April, when the asteroid's phase was lower than on 19th April when we had observed.…”

Section: The Light Curvesupporting

confidence: 82%

Time and Phase Resolved Optical Spectra of Potentially Hazardous Asteroid 2014 JO25

Venkataramani

Ganesh

Rai

et al. 2019

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The asteroid 2014 JO25, considered to be "potentially hazardous" by the Minor Planet Center, was spectroscopically followed during its close-Earth encounter on 19th and 20th of April 2017. The spectra of the asteroid were taken with the low resolution spectrograph (LISA), mounted on the 1.2-m telescope at the Mount Abu Infrared Observatory, India. Coming from a region close to the Hungaria population of asteroids, this asteroid follows a comet-like orbit with a relatively high inclination and large eccentricity. Hence, we carried out optical spectroscopic observations of the asteroid to look for comet-like molecular emissions or outbursts. However, the asteroid showed a featureless spectrum, devoid of any comet-like features.The asteroid's light curve was analyzed using V band magnitudes derived from the spectra and the most likely solution for the rotation of the asteroid was obtained. The absolute magnitude H and the slope parameter G were determined for the asteroid in V filter band using the IAU accepted standard two parameter H-G model. A peculiar, rarely found result from these observations is its phase bluing trend. The relative B-V color index seems to decrease with increasing phase angle, which indicates a phase bluing trend. Such trends have seldom been reported in literature. However, phase reddening in asteroids is very common. The asymmetry parameter g and the single scattering albedo w were estimated for the asteroid by fitting the Hapke phase function to the observed data. The asteroid shows relatively large value for the single scattering albedo and a highly back scattering surface.

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