Mission design of DESTINY<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline" id="d1e1074" altimg="si23.svg"><mml:msup><mml:mrow/><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msup></mml:math>: Toward active asteroid (3200) Phaethon and multiple small bodies

Ozaki, Naoya; Yamamoto, Takayuki; Gonzalez-Franquesa, Ferran; Gutierrez-Ramon, Roger; Pushparaj, Nishanth; Chikazawa, Takuya; Tos, Diogene Alessandro Dei; Çelik, Onur; Marmo, Nicola; Kawakatsu, Yasuhiro; Arai, Tomoko; Nishiyama, Kazutaka; Takashima, Takeshi

doi:10.1016/j.actaastro.2022.03.029

Cited by 34 publications

(12 citation statements)

References 28 publications

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“…A disruptive trigger event-for example, from rotational instability or a large impact exposing subsurface material-must necessarily have reset the surface volatility to initiate any Nasupported Geminids formation. The upcoming DESTINY + flyby mission aims to provide resolved imaging of Phaethon's surface that could yield clearer evidence for such phenomena (Arai et al 2018;Ozaki et al 2022).…”

Section: Sodium As a Tracer For Mass Lossmentioning

confidence: 99%

Sodium Brightening of (3200) Phaethon near Perihelion

Zhang

Battams

et al. 2023

Planet. Sci. J.

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Sunskirting asteroid (3200) Phaethon has been repeatedly observed in Solar Terrestrial Relations Observatory (STEREO) Heliospheric Imager 1 (HI1) imagery to anomalously brighten and produce an antisunward tail for a few days near each perihelion passage, phenomena previously attributed to the ejection of micron-sized dust grains. Color imaging by the Solar and Heliospheric Observatory (SOHO) Large Angle Spectrometric Coronagraph (LASCO) during the 2022 May apparition indicates that the observed brightening and tail development instead capture the release of sodium atoms, which resonantly fluoresce at the 589.0/589.6 nm D lines. While HI1's design bandpass nominally excludes the D lines, filter degradation has substantially increased its D line sensitivity, as quantified by the brightness of Mercury’s sodium tail in HI1 imagery. Furthermore, the expected fluorescence efficiency and acceleration of sodium atoms under solar radiation readily reproduce both the photometric and morphological behaviors observed by LASCO and HI1 during the 2022 apparition and the 17 earlier apparitions since 1997. This finding connects Phaethon to the broader population of sunskirting and sungrazing comets observed by SOHO, which often also exhibit bright sodium emission with minimal visible dust, but distinguishes it from other sunskirting asteroids without detectable sodium production under comparable solar heating. These differences may reflect variations in the degree of sodium depletion of near-surface material and thus the extent and/or timing of any past or present resurfacing activity.

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Section: Sodium As a Tracer For Mass Lossmentioning

confidence: 99%

Sodium Brightening of (3200) Phaethon near Perihelion

Zhang

Battams

et al. 2023

Planet. Sci. J.

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“…Spectroscopy and colors have been measured extensively (most recently by Lin et al 2020). The Japanese space agency JAXA's forthcoming DESTINY + mission is expected to fly by Phaethon in 2024 (Ozaki et al 2022).…”

Section: Phaethonmentioning

confidence: 99%

Surface Properties of Near-Sun Asteroids

Holt¹,

Knight²,

Kelley³

et al. 2022

Planet. Sci. J.

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Near-Earth asteroids (NEAs) with small perihelion distances reach subsolar temperatures of ≥1000 K. They are hypothesized to undergo “supercatastrophic” disruption, potentially caused by near-Sun processes such as thermal cracking, spin-up, meteoroid impacts, and subsurface volatile release, all of which are likely to cause surface alteration, which may change the spectral slope of the surface. We attempted to observe 35 of the 53 known near-Sun asteroids with q ≤ 0.15 au from 2017 January to 2020 March to search for trends related to near-Sun processes. We report the optical colors and spectral slopes of 22 objects that we successfully observed and the measured rotation periods for three objects. We find the distribution of colors to be overall bluer than the color distribution of NEAs, though there is a large overlap. We attribute the large scatter to unknown dynamical histories and compositions for individual objects, as well as competing surface altering processes. We also investigated potential correlations between colors and other properties (e.g., perihelion distance, Tisserand parameter, rotation period) and searched for evidence of activity. Finally, we have compiled all known physical and dynamical properties of these objects, including probabilistic source regions and dwell times with q ≤ 0.15 au.

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“…JAXA's DESTINY + mission plans a Phaethon flyby at a relative speed of 36 km s −1 either in 2028 January or 2030 November, with a closest approach distance of about 500 km (Ozaki et al 2022). The DESTINY + dust analyzer (DDA) has the two sensor heads with a total sensitive area, A DDA = 0.035 m 2 , for collecting interplanetary dust particles with radii 10 μm (a particle mass 10 −11 kg; Krüger et al 2019).…”

Section: Destiny + Updatementioning

confidence: 99%

“…Another motivation is to find an activity mechanism far from perihelion, which is different from thermally related production. This study provides a groundwork for JAXA's DESTINY + mission, which is planning to fly by at a distance of 500 km from Phaethon in 2028, with a potential extended mission to fly by 2005 UD (Ozaki et al 2022).…”

Section: Introductionmentioning

confidence: 99%

WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC

Kasuga

Masiero

2022

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We present space-based thermal infrared observations of the presumably Geminid-associated asteroids: (3200) Phaethon, 2005 UD, and 1999 YC using Wide-field Infrared Survey Explorer/Near-Earth Object WISE. The images were taken at the four wavelength bands 3.4 μm (W1), 4.6 μm (W2), 12 μm (W3), and 22 μm (W4). We find no evidence of lasting mass loss in the asteroids over the decadal multiepoch data sets. We set an upper limit to the mass-loss rate in dust of Q dust ≲ 2 kg s−1 for Phaethon and ≲0.1 kg s−1 for both 2005 UD and 1999 YC, respectively, with little dependency over the observed heliocentric distances of R h = 1.0–2.3 au. For Phaethon, even if the maximum mass loss was sustained over the 1000(s) yr dynamical age of the Geminid stream, it is more than two orders of magnitude too small to supply the reported stream mass (1013–14 kg). The Phaethon-associated dust trail (Geminid stream) is not detected at R h = 2.3 au, corresponding to an upper limit on the optical depth of τ < 7 × 10−9. Additionally, no comoving asteroids with radii r e < 650 m were found. The DESTINY+ dust analyzer would be capable of detecting several of the 10 μm sized interplanetary dust particles when at far distances (≳50,000 km) from Phaethon. From 2005 UD, if the mass-loss rate lasted over the 10,000 yr dynamical age of the Daytime Sextantid meteoroid stream, the mass of the stream would be ∼1010 kg. The 1999 YC images showed neither the related dust trail (the optical depth τ < 2 × 10−8) nor comoving objects with radii r e < 170 m at R h = 1.6 au. Estimated physical parameters from these limits do not explain the production mechanism of the Geminid meteoroid stream. Lastly, to explore the origin of the Geminids, we discuss the implications for our data in relation to the possibly sodium-driven perihelion activity of Phaethon.

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Mission design of DESTINY+: Toward active asteroid (3200) Phaethon and multiple small bodies

Cited by 34 publications

References 28 publications

Sodium Brightening of (3200) Phaethon near Perihelion

Sodium Brightening of (3200) Phaethon near Perihelion

Surface Properties of Near-Sun Asteroids

WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC

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