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Contents

162173 1999 JU3Edit

  • Vilas, Faith (2008). "Spectral Characteristics of Hayabusa 2 Near-Earth Asteroid Targets 162173 1999 Ju3 and 2001 Qc34". The Astronomical Journal. 135 (4): 1101. doi:10.1088/0004-6256/135/4/1101.
  • Hasegawa, Sunao; Müller, Thomas G.; Kawakami, Kyoko; Kasuga, Toshihiro; Wada, Takehiko; Ita, Yoshifusa; Takato, Naruhisa; Terada, Hiroshi; Fujiyoshi, Takuya; Abe, Masanao. "Albedo, Size, and Surface Characteristics of Hayabusa-2 Sample-Return Target 162173 1999 JU3 from AKARI". Publications of the Astronomical Society of Japan. 60 (SP2): S399–S405.CS1 maint: Multiple names: authors list (link)
  • Abe, Masanao; Kawakami, Kyoko; Hasegawa, Sunao; Kuroda, Daisuke; Yoshikawa, Makoto; Kasuga, Toshihiro; Kitazato, Kohei; Sarugaku, Yuki; Kinoshita, Daisuke; Miyasaka, Seidai; Urakawa, Seitaro; Okumura, Shinichirou; Takagi, Yasuhiko; Takato, Naruhisa; Fujiyoshi, Takuya; Terada, Hiroshi; Wada, Takehiko; Ita, Yoshifusa; Vilas, Faith; Weissman, Paul; Choi, Young-Jun; Larson, Steve; Bus, Schelte; Mueller, Thomas (13–20 July 2008). Ground-based observational campaign for asteroid 162173 1999 JU3 (PDF). 37th COSPAR Scientific Assembly. Montréal, Canada.CS1 maint: Multiple names: authors list (link) CS1 maint: Date format (link)
  • Campins, H.; Emery, J. P.; Kelley, M.; Fernández, Y.; Licandro, J.; Delbó, M.; Barucci, A.; Dotto, E. (2009). "Spitzer observations of spacecraft target 162173 (1999 JU3)" (PDF). Astronomy and Astrophysics. 503 (2): L17. doi:10.1051/0004-6361/200912374.
  • GROUND-BASED OBSERVATIONAL CAMPAIGN FOR ASTEROID 162173 1999 JU3 (PDF). Lunar and Planetary Science XXXIX. League City, Texas. March 10–14, 2008. p. 1594. Text " 39th Lunar and Planetary Science Conference, (Lunar and Planetary Science XXXIX) " ignored (help); Text " 1391 " ignored (help)CS1 maint: Date format (link)
  • Vilas, Faith (2008). "SPECTRAL CHARACTERISTICS OF HAYABUSA 2 NEAR-EARTH ASTEROID TARGETS 162173 1999 JU3 AND 2001 QC34". The Astronomical Journal. 135 (4): 1101. doi:10.1088/0004-6256/135/4/1101.
  • "International Symposium Marco Polo and other Small Body Sample Return Missions".

MascotEdit

Instruments / explosion and penetratorEdit

The statement "The explosion will form a copper penetrator hitting the asteroid with a velocity of 2 km/s" is unclear. Perhaps something like "The copper penetrator's velocity of 2 km/s will create an explosion due to the kinetic energy of its impact."? 128.170.224.10 (talk) 20:16, 8 December 2014 (UTC)daddyodel

No - the high explosive forms the (liquid?) copper penetrator and accelerates it to 2km/s. - Rod57 (talk) 14:44, 13 September 2017 (UTC)

2014 XX39Edit

Is it worth mentioning in the article that Hayabusa 2 was discovered as near-Earth asteroid 2014 XX39?

-- Kheider (talk) 22:40, 6 January 2015 (UTC)

Clarification question. The Hayabusa 2 probe was misidentified as a near-miss asteroid as it left Earth orbit, and was later identified as being the space probe? Maybe that would be more appropriate for a page on detecting Near Earth Objects rather than cluttering up information about the Hayabusa 2 mission.
PoqVaUSA (talk) 16:08, 10 March 2015 (UTC)
Actually, the 1999 JU3 asteroid for the Hayabusa 2 mission and the Itokawa (1998 SF36) asteroid for the original Hayabusa mission are both considered Potentially Hazardous Asteroids (PHAs).
* http://neo.jpl.nasa.gov/orbits/
So maybe there would be an interest on the Hayabusa 2 page for a comment about efforts to detect Near Earth Asteroids (NEAs) in general, and PHAs in particular, with a link to a page with more detail about the current state of the art.
PoqVaUSA (talk) 16:31, 10 March 2015 (UTC)
I'm not totally sold on the notability of this info- seems kind of like trivia, with little impact to the mission. But if there's a verifiable source per WP:V (i.e. not just a posting on a groups.yahoo.com forum), perhaps there's a way to include the info. I would stick to how this relates to Hayabusa 2, however. A general comment about detecting NEAs/PHAs belongs in a different article. Cheers! Skyraider1 (talk) 01:49, 11 March 2015 (UTC)

What is MINERVAEdit

MINERVA is mentioned in the infobox, but not described ? - Rod57 (talk) 14:46, 13 September 2017 (UTC)

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External links modified (January 2018)Edit

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SampleEdit

There is no information whatsoever on how the sample will be collected and how it will be sent to Earth. Rowan Forest (talk) 22:06, 18 June 2018 (UTC)

Sampling is documented now, but the article is still missing info on how the samples will be sent toward Earth and how they will be retrieved. Rowan Forest (talk) 19:14, 21 September 2018 (UTC)
@Rowan Forest: Not sure this will help, but here's a entry about the sampling in general titled C 型小惑星をもちかえる(Bringing back a C-type asteroid) written by Shogo Tachibana, who was Sampler team lead for Hayabusa2. It was originally on a academic paper published by the Japanese Society for Planetary Science, and was reprinted on this website. Kind regards, Hms1103 (talk) 07:40, 24 September 2018 (UTC)
@Hms1103: Do you know which section in that paper deals with the return trip and sample return? I could use an automated translator for that specific section. 3 samples total = one from surface two from the excavated crater? Any sample curation during transport? Parachute descent? Which facility will process the samples? Also, can you find info on the specifications of the ion engines? Thanks, Rowan Forest (talk) 14:03, 24 September 2018 (UTC)
Can you confirm that in Section 4 the 3 samplings are: 1) dry regolith, 2) hydrated regolith (or bedrock if wet regolith can't be found), 3) subsurface sample from the crater excavated by the bullet. Thank you, Rowan Forest (talk) 14:25, 24 September 2018 (UTC)
@Rowan Forest: In section 4, it mentions that The first candidate is regolithic surface that exhibits traits of hydrous minerals( 含水鉱物の特徴が確認できるレゴリス状表面). Other candidates are places that evidence of aqueous alterations is either unobservable or weak(水質変成の証拠がみえないか弱い地点). If the surface doesn't show diversity in materials(表面に物質の多様性が認められない場合), sampling from the bedrock becomes a candidate. The third sampling will take place at the excavated crater, where it is expected that samples with a minimum effect from surface process will be gained. A), B), C), describes the type of samples that they want to collect from a scientific perspective(they want samples of each of them), and the regolithic surface that exhibits traits of hydrous minerals may have all three of it.
Any sample curation during transport? →In section 4's (4), it mentions that they are planning to collect volatile sample component prior to unsealing the sample container. Also, in (3) it says that the sample container is sealed as such that on Earth, less than 1Pa of atmosphere leaks inside per week. Which facility will process the samples? →The short answer is, here, at the Extraterrestrial Sample Curation Center, which is inside JAXA Sagamihara Campus. In the article, towards the end of section4 it says that they expect to conduct element/isotope analysis, mineral and textural observation, gas analysis and organic analysis.
Some specs of the ion engine are shown here [1]. Regards, Hms1103 (talk) 08:18, 25 September 2018 (UTC)
The automated translations can be tricky, so thank you for the info on the sampling and on the engines. It is appreciated. Rowan Forest (talk) 14:00, 25 September 2018 (UTC)

A Commons file used on this page has been nominated for deletionEdit

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