TY - JOUR
T1 - UV to near-IR obser vãtions of the DART-Dimorphos collision
AU - Ofek, Eran O.
AU - Kushnir, Doron
AU - Polishook, David
AU - Waxman, Eli
AU - Tohuvavohu, Aaron
AU - Ben-Ami, Sagi
AU - Katz, Boaz
AU - Gnat, Orly
AU - Strotjohann, Nora L.
AU - Segre, Enrico
AU - Blumenzweig, Arie
AU - Sofer-Rimalt, Yahel
AU - Yaron, Ofer
AU - Gal-Yam, Avishay
AU - Shvartzvald, Yossi
AU - Engel, Michael
AU - Cenko, S. Bradley
AU - Hershko, Ofir
N1 - Publisher Copyright:
© 2023 The Author(s).
PY - 2024/2/1
Y1 - 2024/2/1
N2 - The impact of the Double Asteroid Redirection Test (DART) spacecraft with Dimorphosãllows us to studyãsteroid collision physics, including momentum transfer, the ejecta properties,ãnd the visibility of such events in the Solar system. We report observations of the DART impact in the ultraviolet (UV), visible light,ãnd near -infrared (IR) wa velengths. The observations support the existence ofãt least two separate components of the ejecta:ã fastãndã slow component. The fast-ejecta component is composed ofã gaseous phase, movingãtãbout 1.6 km s -1 withã mass of ≲10 4 kg. The fast ejecta is detected in the UVãnd visible light, but not in the near-IR z-band observations. Fittingã simplified optical thickness model to these observationsãllows us to constrain some of the properties of the fast ejecta, including its scattering efficiencyãnd the opacity of the gas. The slow ejecta component is movingãt typical velocities of up toãbout 10 m s -1 . It is composed of micrometer-size particles, that haveã scattering efficiency,ãt the direction of the observer, of the order of 10 -3ãndã total mass of ∼10 6 kg. The larger particles in the slow ejecta, whose size is bound to be in the range between ∼1 mmãnd ∼1 m, likely haveã scattering efficiency larger than that of the pre-impact Didymos system.
AB - The impact of the Double Asteroid Redirection Test (DART) spacecraft with Dimorphosãllows us to studyãsteroid collision physics, including momentum transfer, the ejecta properties,ãnd the visibility of such events in the Solar system. We report observations of the DART impact in the ultraviolet (UV), visible light,ãnd near -infrared (IR) wa velengths. The observations support the existence ofãt least two separate components of the ejecta:ã fastãndã slow component. The fast-ejecta component is composed ofã gaseous phase, movingãtãbout 1.6 km s -1 withã mass of ≲10 4 kg. The fast ejecta is detected in the UVãnd visible light, but not in the near-IR z-band observations. Fittingã simplified optical thickness model to these observationsãllows us to constrain some of the properties of the fast ejecta, including its scattering efficiencyãnd the opacity of the gas. The slow ejecta component is movingãt typical velocities of up toãbout 10 m s -1 . It is composed of micrometer-size particles, that haveã scattering efficiency,ãt the direction of the observer, of the order of 10 -3ãndã total mass of ∼10 6 kg. The larger particles in the slow ejecta, whose size is bound to be in the range between ∼1 mmãnd ∼1 m, likely haveã scattering efficiency larger than that of the pre-impact Didymos system.
KW - minor planets: individual: Didymos
KW - minor planets: individual: Dimorphos
UR - http://www.scopus.com/inward/record.url?scp=85183418768&partnerID=8YFLogxK
U2 - 10.1093/mnras/stad3707
DO - 10.1093/mnras/stad3707
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AN - SCOPUS:85183418768
SN - 0035-8711
VL - 527
SP - 10507
EP - 10521
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -