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# Near-Ultraviolet and Visible Spectroscopy of HAYABUSA Spacecraft Re-entry

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## Abstract and Figures

HAYABUSA is the first spacecraft ever to land on and lift off from any celestial body other than the moon. The mission, which returned asteroid samples to the Earth while overcoming various technical hurdles, ended on 2010 June 13, with the planned atmospheric re-entry. In order to safely deliver the sample return capsule, the HAYABUSA spacecraft ended its 7-year journey in a brilliant artificial fireball'' over the Australian desert. Spectroscopic observation was carried out in the near-ultraviolet and visible wavelengths between 3000 Å and 7500 Å at 3–20 Å resolution. Approximately 100 atomic lines such as Fe i, Mg i, Na i, Al i, Cr I, Mn i, Ni i, Ti i, Li i, Zn i, O i, and N i were identified from the spacecraft. Exotic atoms such as Cu i, Mo i, Xe i and Hg i were also detected. A strong Li i line (6708 Å) at a height of $\sim\$55 km originated from the onboard Li-Ion batteries. The FeO molecule bands at a height of $\sim\$63 km were probably formed in the wake of the spacecraft. The effective excitation temperature as determined from the atomic lines varied from 4500 K to 6000 K. The observed number density of Fe i was about 10 times more abundant than Mg i after the spacecraft explosion. N$_{2}^{+}$ ($1^-$) bands from a shock layer and CN violet bands from the sample return capsule's ablating heat shield were dominant molecular bands in the near-ultraviolet region of 3000–4000 Å. OH($A$–$X$) band was likely to exist around 3092 Å. A strong shock layer from the HAYABUSA spacecraft was rapidly formed at heights between 93 km and 83 km, which was confirmed by detection of N$_{2}^{+}$ ($1^-$) bands with a vibration temperature of $\sim\$13000 K. Gray-body temperature of the capsule at a height of $\sim\$42 km was estimated to be $\sim\$2437 K which is matched to a theoretical prediction. The final message of the HAYABUSA spacecraft and its sample return capsule are discussed through our spectroscopy.
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arXiv:1108.5982v1 [astro-ph.EP] 30 Aug 2011
Near-Ultraviolet and Visible Spectroscopy of
HAYABUSA Spacecraft Re-entry
Shinsuke Abe
National Central University, 300 Jhongda Road, Jhongli, Taoyuan 32001, Taiwan
shinsuke.avell@gmail.com
Kazuhisa Fujita
Japan Aerospace Exploration Agency, 7-44-1 Jinidaiji-higashi-machi, Chofu, Tokyo 182-8522, Japan
fujita.kazuhisa@jaxa.jp
Yoshihiro Kakinami
Institute of Seismology and Volcanology, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo
060-0810, Japan
kakinami@mail.sci.hokudai.ac.jp
Ohmi Iiyama
Osaka Science Museum, 4-2-1 Nakanoshima, Kitaku, Osaka, Osaka 530-0005, Japan
Hirohisa Kurosaki
Japan Aerospace Exploration Agency, 7-44-1 Jinidaiji-higashi-machi, Chofu, Tokyo 182-8522, Japan
Michael A. Shoemaker
Kyushu University, 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan
Yasuo Shiba and Masayoshi Ueda
Nippon Meteor Society, 43-2 Asuka Habikino Osaka 583-0842, Japan
and
Masaharu Suzuki
GOTO Inc., 4-16 Yazaki-cho, Fuchu, Tokyo 183-8530, Japan
(Received 2011 June 23; accepted 2011 August 28)
Abstract
HAYABUSA is the ﬁrst spacecraft ever to land on and lift oﬀ from any celestial
body other than the moon. The mission, which returned asteroid samples to the
Earth while overcoming various technical hurdles, ended on June 13, 2010, with the
planned atmospheric re-entry. In order to safely deliver the sample return capsule,
the HAYABUSA spacecraft ended its 7-year journey in a brilliant “artiﬁcial ﬁreball”
over the Australian desert. Spectroscopic observation was carried out in the near-
ultraviolet and visible wavelengths between 3000 and 7500 ˚
A at 3 – 20 ˚
A resolution.
Approximately 100 atomic lines such as Fe I, Mg I, Na I, Al I, Cr I, Mn I, Ni I, Ti I, Li I,
Zn I, O I, and N Iwere identiﬁed from the spacecraft. Exotic atoms such as Cu I, Mo I,
1
Xe Iand Hg Iwere also detected. A strong Li Iline (6708 ˚
A) at a height of 55 km
originated from the onboard Li-Ion batteries. The FeO molecule bands at a height of
63 km were probably formed in the wake of the spacecraft. The eﬀective excitation
temperature as determined from the atomic lines varied from 4500 K to 6000 K. The
observed number density of Fe Iwas about 10 times more abundant than Mg Iafter
the spacecraft explosion. N+
2(1) bands from a shock layer and CN violet bands
from the sample return capsule’s ablating heat shield were dominant molecular bands
in the near-ultraviolet region of 3000 – 4000 ˚
A. OH(A-X) band was likely to exist
around 3092 ˚
A. A strong shock layer from the HAYABUSA spacecraft was rapidly
formed at heights between 93 km and 83 km, which was conﬁrmed by detection of
N+
2(1) bands with a vibration temperature of 13000 K. Gray-body temperature
of the capsule at a height of 42 km was estimated to be 2437 K which is matched
to a theoretical prediction. The ﬁnal message of the HAYABUSA spacecraft and its
sample return capsule are discussed through our spectroscopy.
Key words: Meteors, meteoroids – asteroid – atmospheric re-entry – spectroscopy
1. Introduction
HAYABUSA, the third engineering space mission of JAXA/ISAS (Japan Aerospace
eXploration Agency/Institute of Space and Astronautical Sciences) had several engineering
technologies to verify in space (e.g, Kawaguchi, Fujiwara & Uesugi 2008). HAYABUSA was
launched on May 9, 2003. On September 12, 2005, HAYABUSA arrived at the asteroid (25143)
Itokawa. The mission was the ﬁrst to reveal that Itokawa is a rubble-pile body rather than
a single monolithic asteroid among S-class asteroids (Abe et al. 2006; Fujiwara et al. 2006).
Finally, the spacecraft performed a landing on Itokawa to collect asteroid samples in November,
2005. Due to a loss of communications, HAYABUSA started an orbit transfer to return to the
Earth in April, 2007. The round-trip travel between the Earth and Itokawa with the aid of ion
engine propulsion was the ﬁrst success of its kind in the world (Kuninaka 2008).
On June 13, 2010, the HAYABUSA spacecraft returned to the Earth with the re-entry
capsule containing asteroid samples. The sample return capsule was separated at 10:51 UT,
which was just 3 hours before the atmospheric re-entry. Due to the failure of all bi-propellant
thrusters for orbital maneuvering, the HAYABUSA spacecraft could not escape from its Earth
collision course. Though Japan had several successful experiences with re-entry capsule tests
(e.g., RFT-2 (1992), OREX (1994), EXPRESS (1995), HYFREX (1996), and USERS (2003)),
the HAYABUSA sample return capsule was the ﬁrst Japanese re-entry opportunity that entered
the Earth’s atmosphere directly from an interplanetary transfer orbit with a velocity over 12
km/s. The HAYABUSA sample return capsule and the spacecraft entered the atmosphere at
2
Table 1. Speciﬁcations of spectroscopic and imaging cameras.
Name Color Lens Spectrograph FOV (H ×V) Pixels Frame rate
VIS-HDTV Color 80mm/f5.6 300 /mm25×171920 ×1080 30 fps
UV-II B/W 30mm/f1.2 600 /mm23×13720 ×480 29.97 (NTSC)
NCR-550aColor 4.6 – 60 mm 90– 8diagonal 800 ×412 29.97 (NTSC)
Nikon D300sColor 18 – 200mm 10×71280 ×720 24 fps
WAT-100N∗∗ B/W 25mm/f0.95 15×11768 ×494 29.97 (NTSC)
Spectrum resolution = 12˚
A (1st order), 6˚
A (2nd order) & 3˚
A (3rd order).
Spectrum resolution = 20˚
A.
Video data was published on the JAXA digital archive; http://jda.jaxa.jp
∗∗ Video data is used for the trajectory estimation of fragmented HAYABUSA (Shoemaker et al. 2011).
13:51 UT. The HAYABUSA spacecraft disintegrated in the atmosphere, and the capsule ﬂew
nominally and landed approximately 500 m from its targeted landing point.
Spectroscopy of the HAYABUSA re-entry was a golden opportunity to understand (i)
the atmospheric inﬂuence upon Earth impactors such as meteors, meteorites and meter-sized
mini-asteroids, because for such natural bodies the original material, mass, and shape are all
unknown (e.g., Ceplecha et al. 1996; Abe 2009); for HAYABUSA, not only these parameters
but also the re-entry trajectory were under perfect control, (ii) the hypervelocity impact of large
objects that are diﬃcult to reproduce in laboratory experiments, and (iii) the ﬂight environment
of re-entry capsules for the utilization of future Japanese sample return missions.
2. Observation and data reduction
A ground observation team consisting of 16 members was organized by JAXA (Fujita
et al. 2011a). Triangulation observations were coordinated between GOS3 station at Tarcoola
(134.55858 E, –30.699114 S, 0.152 km altitude) and GOS4 station at Coober Pedy (134.71819
E, –29.03392 S, 0.224 km altitude) in southern Australia (ﬁgure 1). The National Astronomical
Observatory of Japan (NAOJ) also made a HAYABUSA observing expedition at Coober Pedy
(see Watanabe et al. 2011).
Spectroscopy was carried out using two spectrograph systems: a VISual HDTV camera
(VIS-HDTV) and an UltraViolet Image-Intensiﬁed TV camera (UV-II). An EOS 5D MarkII
with lens (f=80mm, f/5.6) was applied to the VIS-HDTV system equipped with a transmission
grating (300 grooves per mm, blazed at 6100 ˚
A). The UV-II system consisted of a UV lens
(f=30mm, f/1.2), a UV image intensiﬁer (φ18-mm photo-cathode: S20), two relay lenses
(f=50mm, f/1.4), and a SONY HDTV Handycam. The UV-II system was equipped with a
reﬂection grating (600 grooves per mm, blazed at 3300 ˚
A). The VIS-HDTV camera obtained
the 0th, 1st, and 2nd order spectra in 4000 – 7000 ˚
A , and the UV-II camera observed the 1st
3
128˚
128˚
130˚
130˚
132˚
132˚
134˚
134˚
136˚
136˚
138˚
138˚
140˚
140˚
−36˚ −36˚
−34˚ −34˚
−32˚ −32˚
−30˚ −30˚
−28˚ −28˚
−26˚ −26˚
0 100
km
AUSTRALIA
Woomera
GOS3 (Tarcoola)
GOS4 (Coober Pedy)
113.2 km
66.9 km
33.2 km
99.4 84.5 62.7
54.9 40.0
Fig. 1. HAYABUSA tra jectory and observation stations in Australia. The HAYABUSA re-entry has
ﬂown over and landed on the Woomera Prohibited Area (WPA) where unauthorized people have no
admittance. GOS sites were located on the border of the WPA. A thick black line shows the trajectory
of sample return capsule in which white dots indicate the heights of beginning (113.2 km), maximum
brightness (66.9 km) and the end (33.2 km) detected by our cameras. Several heights at which the spectra
were analyzed are indicated by the X marks.
4
Table 2. Beginning and terminating of light detected by each camera and corresponding trajectory of HAYABUSA and the
capsule.
Time HeightVelocityEvent Cameras
UT km kms1(SPectrum or IMage)
13:51:50.1 113.21 12.05 Beginning WAT-100N (IM)
13:51:53.5 106.17 12.06 Beginning NCR-550a (IM)
13:51:54.3 104.53 12.06 Beginning UV-II (SP)
13:51:57.8 97.46 12.06 Beginning D300s (IM)
13:52:03.9 85.47 12.07 Beginning VIS-HDTV (SP)
13:52:12.9 68.63 11.95 Explosion all
13:52:13.6 67.38 11.90 Explosion all
13:52:13.9 66.85 11.88 Maximum all
13:52:17.1 61.39 11.57 Explosion all
13:52:17.2 61.22 11.55 Explosion all
13:52:19.5 57.53 11.18 Explosion all
13:52:19.9 56.90 11.10 Explosion all
13:52:22.7 52.79 10.44 Ending VIS-HDTV (SP)
13:52:40.2 36.81 3.38 Ending UV-II (SP)
13:52:42.1 35.98 2.94 Ending D300s (IM)
13:52:47.4 34.09 2.08 Ending NCR550a (IM)
13:52:50.6 33.17 1.74 Ending WAT-100N (IM)
The trajectory of HAYABUSA and the capsule was obtained by our observation (Boroviˇcka et al. 2011).
The velocity relative to the Earth’s center is given (the velocity relative to the surface is about 0.37 km/s
lower because of Earth’s rotation).
order spectrum in 3000 – 7500 ˚
A (ﬁgure 2). A part of the 2nd order spectrum of the VIS-
HDTV was overlapped with the 3rd order spectrum. The speciﬁcations of the spectroscopic
and imaging cameras are summarized in table 1.
The tracking observations at GOS3 were carried out by S. Abe using co-aligned dual
imaging cameras (Nikon D300s and WAT-100N) and the UV-II spectrograph which were
mounted on the same hydraulic tripod. Tracking was performed while watching a video mon-
itor taken by WAT-100N (WATEC Inc.). The high-sensitivity television camera, NCR-550a
(NEC Corp. & GOTO Inc.), equipped with three 1/2 type EM-CCD (Electron Multiplying
CCD) image sensors, was also used to observe the zoomed color TV operated by O. Iiyama. At
GOS4, the VIS-HDTV spectroscopy was achieved by Y. Kakinami adopting the same tracking
method. Meanwhile, 6×7 photographic cameras using a ﬁsh-eye lens with a rotating shut-
ter were operated simultaneously at GOS3 by S. Abe and at GOS4 by Y. Kakinami and Y.
Shiba. In this paper, the most reliable trajectory (time, height, and velocity) determined by
5
0.0
0.2
0.4
0.6
0.8
1.0
3000 4000 5000 6000 7000 8000
Efficiency
Wavelength (Å)
VIS (1st order)
VIS (2nd order)
UV (1st order)
Fig. 2. Eﬃciency curves of the VIS-HDTV and UV-II spectroscopic cameras. The 1st order spectra are
normalized 1.0 at their maximum. The eﬃciency of the 2nd order of the VIS-HDTV is relative to its 1st
order spectrum. The maximum eﬃciency of the UV-II and the VIS-HDTV’s 1st and 2nd orders are 4440,
5804, and 5160 ˚
A, respectively.
our photographic observation is referred (Boroviˇcka et al. 2011). Note that the trajectories
derived from diﬀerent cameras (Shoemaker et al. 2011; Ueda et al. 2011) were comparable
to our result and the JAXA prediction. Tracking the capsule was diﬃcult because although
there were predictions for the time and point in the sky when the objects would ﬁrst appear,
the capsule moved faster and tracking became more diﬃcult later in ﬂight. In order to track
the fast moving HAYABUSA trajectory smoothly, observers were suﬃciently trained by using
an imitation moving laser pointer on the planetarium dome that was arranged by M. Suzuki.
These instrument pointing exercises allowed successful tracking of the HAYABUSA emissions
(Abe 2010).
Background and stars were removed by subtracting a median frame shortly before or
after the spectrum. After ﬂat-ﬁelding and averaging of the HAYABUSA spectrum, the wave-
length was examined carefully using well-known strong atomic lines such as Mg I(5178 ˚
A) and
Na I(5893 ˚
A). The pixels were converted to wavelengths with a simple linear function. After
6
more known lines were identiﬁed, the wavelength was precisely determined again with regard
to the synthetic atomic lines that were convolved by the spectrum resolution (Boroviˇcka 1993).
On the other, spectra of Venus and Canopus (αCar) were used to calculate the eﬃciency curves
for the VIS-HDTV and UV-II cameras, respectively (ﬁgure 2). Table 2 gives trajectories of the
HAYABUSA spacecraft (H >50 km) and the capsule (H<50 km) compared with detections
by our imaging and spectroscopic cameras. The VIS-HDTV spectroscopy was aimed at the
HAYABUSA spacecraft (50<H<85 km), whereas the UV-II spectroscopy was intended to ob-
serve the faint spectrum at the beginning height (H>80 km) and the capsule spectrum near
the terminal height (H<50 km). Here, we selected some of the best data among a series of
spectrum (see ﬁgure 12 in Fujita et al. 2011a).
3. Results
3.1. VIS-HDTV spectrum in 4000 – 7000 ˚
A
Figure 3 shows the VIS-HDTV spectra of the HAYABUSA spacecraft at heights of 84.5,
62.7, and 54.9 km. The estimated absolute magnitude at each height were –7, –12, and –8,
respectively. Note that the absolute magnitude is deﬁned as the magnitude an object would have
as if placed at the observer’s zenith at a height of 100 km. Corresponding color images taken
with the NCR-550a and the Nikon D300s were compared. These spectra were not calibrated
by the sensitivity curve so that they could be compared with the color as seen by an average
human eye as well as with the color images. Identiﬁed atoms were indicated on the top of
each emission. After the spectral response calibration, the 1st and the 2nd order spectra were
obtained (ﬁgure 4). Most of the 1st order spectra of the VIS-HDTV and the UV-II during the
explosion phase were saturated in their intensities. The 2nd order spectra of the VIS-HDTV,
fortunately, were free from saturation and were worthy of close inspection. The absolute ﬂux
was estimated using the unsaturated 2nd order spectrum when the maximum magnitude of –
12.6 was reached at a height of 66.9 km (Boroviˇcka et al. 2011). Identiﬁed atoms and molecules
using the VIS-HDTV are summarized in table 6.
At a height of 84.5 km, Mg I(5173 and 5184 ˚
A) and Na I(5890 and 5896 ˚
A) emissions
were dominant. During the explosion phase, numerous strong emissions were seen in the visible
spectrum. Some exotic lines were detected, such as Cu I(5700 and 5782 ˚
A), Mo I(5506 and
5533 ˚
A), Xe I(4624 and 4671 ˚
A), and Hg I(4358 and 5461 ˚
A), which typically could not be
seen in a natural meteor spectrum. Note that the “duralumin” of HAYABUSA’s structure
contains Al, Cu, Mg, and Mn. MoS2(molybdenum disulﬁde) was used as a lubricant in many
places of the spacecraft. HAYABUSA’s propulsion system operated by accelerating ionized Xe
(xenon gas) through a strong electric ﬁeld, and expelling it at high speed. Of the total 66 kg
of xenon gas that was carried on HAYABUSA, there remained about 10 kg at the time of the
Earth return. Xe Iat 4671 ˚
A was clearly seen in the spectrum (H=62.7 km) after the main
7
Fig. 3. Visible spectrum of HAYABUSA spacecraft compared with color images taken by the NCR-550a
(NEC Corp. & GOTO Inc.) forming a background and the Nikon D300s in a rectangular box. Identiﬁed
atomic lines are indicated atop each emission. ’?’ marks are unknown (unidentiﬁed) lines. A color spec-
trum as seen by an average human eye is shown (Nick Spiker; http://www.repairfaq.org/sam/repspec/).
explosion, and disappeared at a lower height (H=54.9 km). The strong Li Ilines (6104 and
6708 ˚
A) at a height of 54.9 km were detected from the spectrum of the HAYABUSA spacecraft.
It is most likely that the observed Li Iemissions originated from the Li-Ion batteries consisting
of 11 prismatic cells with 6.3 kg total mass onboard the HAYABUSA spacecraft. A series
of strong Zn Ilines (4680, 4722, and 4811 ˚
A) were detected that was probably originated from
the spacecraft. Similar Zn Ilines have been seen in a “paint” spectrum of the NASA Stardust
capsule due to paint that was applied to the surface of the capsule (Abe et al. 2007a; Jenniskens
2010a).
The continuum spectral proﬁle around 6000 ˚
A at a height of 62.7 km is very similar to
published laboratory measurements of the “orange bands” of FeO which have been detected by
Jenniskens (2000) and Abe et al. (2005a) in Leonid meteor persistent trains. FeO is the most
common molecule observed in the spectrum of bright and relatively slow ﬁreballs (Ceplecha
8
0
100
200
300
400
4200 4400 4600 4800 5000 5200 5400 5600 5800 6000 6200 6400 6600 6800 7000
Flux (10−9 W m−2 nm−1)
Wavelength (Å)
2nd order
H=62.7km (13:52:16.3 UT)
H=54.9km (13:52:21.2 UT)
FeO (Jenniskens, 2000)
0
20
40
60 1st order
H=84.5km (13:52:04.4 UT)
H=54.9km (13:52:21.2 UT)
Fig. 4. The VIS-HDTV spectra of the HAYABUSA spacecraft in the 1st (upper panel) and in the 2nd
(lower panel) order after spectral sensitivity calibration. The 2nd order spectrum was not obtained for
H=84.5 km due to its faintness, while the 1st order spectrum was mostly saturated for H=62.7 km. The
spectral match with the laboratory spectrum of the FeO orange bands (Jenniskens 2000) is superposed.
Since the 3rd order is clearly mixed with the 2nd order spectrum below 6600 ˚
A , the 3rd order spectrum
is omitted.
1971; Boroviˇcka 1993). The FeO can be formed during the cooling phase when the temperature
drops to 2500 – 2000 K (Berezhnoy & Boroviˇcka 2010), thus it may be emitted in the wake of
the HAYABUSA spacecraft. Recently, FeO has been discovered in a terrestrial night airglow
spectrum observed with the Odin spacecraft (Evans et al. 2010).
3.2. UV-II spectrum in 3000 – 4000 ˚
A
Figure 5 shows a series of the UV-II spectra for the spacecraft-capsule mixed at heights
between 99.4 km – 82.9 km and for the capsule at heights between 44.7 km – 39.6 km before
spectral sensitivity calibration. N+
2(1) at 3908 ˚
A was a signiﬁcant band head during the
beginning phase, and during the later phase the near-ultraviolet region was ﬁlled with N+
2(1)
bands whose band heads were 3880 and 3533 ˚
A. Figure 6 shows the UV-II spectra at heights of
92.5 km and 82.9 km after sensitivity calibration. A scaled 3rd order spectrum obtained using
9
Table 3. Identiﬁcation of atoms and molecules in 3000 – 4000 ˚
A. Identiﬁed atoms here were based on the spacecraft-capsule
mixed spectrum at a height of 82.9 km (13:52:05 UT), while molecular bands resulted from the spacecraft-capsule mixed
spectra at a height of 92.5 km (13:52:00 UT), 82.9 km (13:52:05 UT), and 62.7 km (13:52:16 UT). Identiﬁed atoms and
synthetic molecular spectra are shown in the UV-II spectrum (ﬁgure 6). The precision of the temperature estimation is
Identiﬁed line
Wavelength (˚
A) Tv=Tr(K)
3092 2000 OH system (A2Σ+X2Π)
3294 4000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3560 4000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3908 4000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3292 13000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3533 13000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3880 13000 N+
2(1) system (B2Σ+
uX2Σ+
g)
3585 13000 CN violet system (B2Σ+X2Σ+)
3849 13000 CN violet system (B2Σ+X2Σ+)
Identiﬁed line
Wavelength (˚
A) Element multiplet Wavelength (˚
A) Element multiplet
3020 Fe I9 3434 Ni I19
3021 Fe I9 3441 Fe I6
3091 Mg I5 3441 Fe I6
3092 Fe I28 3444 Fe I6
3093 Al I3 3446 Ni I20
3093 Al I3 3648 Fe I23
3134 Ni I25 3687 Fe I21
3226 Fe I155 3944 Al I1
3233 Ni I7 3962 Al I1
3415 Ni I19 3969 Fe I43
3424 Ni I20
10
0
50
100
150
200
250
300
3000 4000 5000 6000 7000 8000 9000 10000
Relative Intensity (a.u.)
Wavelength (Å)
N2+(1−)
CN
Fe I
N2+(1−)
Fe I + Ni I
N2+(1−)
OH
Altitude (UT)
99.4km (13:51:56.8)
96.5km (13:51:58.3)
94.5km (13:51:59.3)
92.5km (13:52:00.3)
82.9km (13:52:05.3)
44.7km (13:52:29.4)
42.7km (13:52:31.4)
41.8km (13:52:32.4)
Fig. 5. A time series of the UV-II spectra of HAYABUSA spacecraft (dotted lines) and the re-entry
capsule (solid lines) before spectral sensitivity calibration. The saturation in intensity reaches near 250 in
this ﬁgure. Some important molecular and atomic species below 4000 ˚
A are indicated atop each emissions.
the VIS-HDTV is superposed on this ﬁgure. The model spectrum of N+
2(1) (B2Σ+
uX2Σ+
g)
system with four bands heads (3300, 3500, 3900 and 4200 ˚
A) caused by diﬀerent vibrational
states were carried out varying the temperatures from 1000 K to 20000 K using the SPRADIAN
numerical code (Fujita & Abe 1997). Assuming that a rotation temperature equals to a vibra-
tion temperature, N+
2(1) bands convolved by the spectral resolution (20 ˚
A) were examined
(ﬁgure 6). The CN violet bands (B2Σ+X2Σ+) and a possible contribution of OH band
(A2Σ+X2Π) were also demonstrated in the same way. N+
2molecules were originated from
the atmospheric gas. CN molecules were produced by a chemical product of ablated carbon
atoms from the heat shield of the capsule and atmospheric nitrogen molecules. Both N+
2and
CN molecules were generated in the shock layer of the body. The derived temperatures of
N+
2(1) bands at heights of 92.5 km and 82.9 km were 4000 K and 13000 K, respectively.
Though most of CN bands were buried under strong N+
2(1) bands, a clear CN band head at
3533 ˚
A was detected which is explained by the vibration temperature of 13000 K. The other
emission features consisted mainly of Fe I, Mg I, Al Iand Ni I. Table 3 gives the identiﬁcation
11
0
100
200
300
400
500
600
700
800
900
3000 3200 3400 3600 3800 4000 4200 4400
Relative Intensity (a.u.)
Wavelength (Å)
... VIS (3rd order)
Al I+Fe I
Fe I
Fe I
Fe I + Ni I
Fe I + Ni I
Ni I Mg I + Fe I + Al I
H=92.5km (13:52:00.3 UT)
H=82.9km (13:52:05.3 UT)
H=62.7km (13:52:16.3 UT)
N2+(1−) ; Tv,r = 4000K
N2+(1−) ; Tv,r = 13000K
CN ; Tv,r = 13000K
OH ; Tv,r = 2000K
Fig. 6. Selected UV-II spectra of HAYABUSA spacecraft after sensitivity calibration compared. The
scaled 3rd order of the VIS-HDTV spectrum without sensitivity calibration is shown in the 3400 – 3600
˚
A range. N+
2(1) bands from a shock layer and CN violet bands from an ablating heat shield of a
sample return capsule are dominant molecular bands. OH(A-X) band is likely to exist around 3092 ˚
A,
but blended with atomic lines. Assuming that a rotation temperature equals to a vibration temperature,
the model spectrum of N+
2(1), CN, and OH(A-X) systems are superposed.
Table 4. Gray-body temperature of the sample return capsule.
Time Height Velocity Temperature
UT km kms1K
13:52:31.35 42.69 6.35 2482 ±11
13:52:32.35 41.81 5.88 2437 ±14
13:52:32.99 41.28 5.58 2395 ±15
of atoms and molecules in the range between 3000 – 4000 ˚
A.
12
1
10
100
1000
4000 4500 5000 5500 6000 6500 7000 7500
Relative Intensity (a.u.)
Wavelength (Å)
H=41.8km, V=5.9km/s (13:52:32.35 UT)
Gray−body temperature = 2437 ± 14 K
Fig. 7. The gray body spectra of the sample return capsule at a height of 42 km. Near-ultraviolet
region below 4500 ˚
A is aﬀected by atom and molecule emissions. Thus, Plank’s formula was applied to
the range between 4500 – 7000 ˚
A as shown.
3.3. Gray-body spectrum of the capsule
A black-body is an idealized object with a perfect absorber and emitter of radiation
whose emissivity is larger than 0.99. An object which has lower emissivity such as a re-entry
capsule is often referred to as a gray-body. The capsule spectrum was well separated from
HAYABUSA’s fragments below 45 km in height while N+
2(1) and CN bands were still strong
in the near-ultraviolet region (ﬁgure 5). After sensitivity calibration, the gray-body temperature
in the wavelengths between 4500 – 6500 (7000) ˚
A was estimated employing Planck’s formula.
The gray-body temperatures of 2482 ±11 K, 2437 ±14 K, and 2395 ±15 K were measured
at heights of 42.7 km, 41.8 km, and 41.2 km, respectively (table 4; ﬁgure 4).
13
Table 5. Derived excitation temperature of radiating gas, the column density and the intensities of identiﬁed main neutral
atoms. The precision of the temperature estimation is about ±500 K, and that of other parameters is within a factor of 2–3.
Height (km) 84.51 62.72 54.94 54.94
Spectrum order 1st 2nd 1st 2nd
T (K) 6000 6000 4500 4500
Mg I1.0E+0 1.0E+0 1.0E+0 1.0E+0
Fe I6.0E-1 1.0E+1 9.0E+0 9.0E+0
Mn I 2.0E-1 3.0E-1 3.0E-1
Ti I<1.0E-3 2.0E-2 2.0E-2 2.0E-2
Na I1.2E-2 1.8E-2 1.0E-3 7.0E-4
Cr I1.2E-2 4.0E-2 4.0E-2 4.0E-2
Li I – 3.2E-3 –
Ni I<1.0E+1 1.0E+1 <1.0E+0 5.0E+0
4. Discussion
4.1. VIS-HDTV spectrum in 4000 – 7000 ˚
A
When the surface temperature of HAYABUSA reached about 2000 K, occurring at a
height around 100 km, the spacecraft material started to sublimate from the surface and was
surrounded by evaporated vapors. Excited states of atoms of these vapors were gradually de-
excited by radiation. HAYABUSA luminosity consisted mostly of radiation of discrete emission
spectral lines belonging under the most part to metals and mainly to iron. Ablation particles
injected into the ﬂow also emitted radiation as a continuum spectrum due to their temperature.
Thus, observed atomic spectrum was mixed with thermal continuum and molecular bands.
Subtracting these background, excitation temperature and element intensities were estimated
under the assumption of a local thermal equilibrium (LTE) condition. Table 5 gives the derived
physical quantities.
The excitation temperature was estimated using Fe Iand Mg Ilines around the 5000
– 5500 ˚
Awavelength range. The derived excitation temperatures were 6000 K at heights of
84.5 km and 62.7 km, and 4500 K at a height of 54.9 km. These excitation temperatures are
comparable to a normal meteor temperature, 5000 K (e.g, Boroviˇcka 1993; Ceplecha et al.
1996; Trigo-Rodriguez et al. 2003) and the excitation temperature range between 5000 K – 6000
K caused by a large bolide (Boroviˇcka et al. 1998). Although the ratio of Fe I/Mg Iwas 0.6 at a
height of 84.5 km, the ratio increased to 10 below a height of 62.7 km. Since HAYABUSA was
made with much more Fe than Mg, it is likely that iron was conspicuously evaporated during
the explosion phase.
Detected Ti Ilines seem to originate from fuel and gas tanks, and also bolts with nuts
14
that were made of Ti-6Al-4V. H Iline (4861 ˚
A) is possibly present, presumably as a result of the
dissociation of N2H4which was used as thruster fuel, meaning that some of the thrusting fuel
remained at re-entry. All other elements (Ni, Cr, and Mn) were probably used for constructing
the HAYABUSA spacecraft. Though Hg Iwas identiﬁed as the most probable element to
explain the presence of lines at 4358 and 5461 ˚
A, details are proprietary information that were
not available to the authors. The detected Na I, especially at heights of 62.7 km and 54.9 km,
is not likely to have originated from the atmosphere; although Earth’s atmosphere contains
natural sodium known as the sodium layer at a height of 80 – 105 km which originated from
meteoroids, this sodium is more rare at these low altitudes. Therefore, sodium must have
originated from material ablated by the HAYABUSA spacecraft or its capsule. Sodium was
also detected by the Stardust capsule at altitudes of 54 – 48 km (Stenbaek-Nielsen & Jenniskens
2010).
OIand N Iare most likely atmospheric lines, or a part of O Iand N Iarising from the
fuel oxidizer, N2O4. O I, N I, H I, and Xe Iare of high excitation atoms which require either high
temperature or a large amount of atoms to be detected. Therefore, these atoms are thought
to be excited by the shock layer. On the other hand, typical lines of the high temperature
components as seen in the meteor plasma such as Mg II (4481 ˚
A) and Fe II (e.g., 4583, 4923,
and 5018 ˚
A) have not been detected in HAYABUSA spectra. The one explanation for the
absence of Mg II and Fe II is that the emissions of O I, N I, H I, and Xe Iarise promptly from
the shock layer in the gas–gas phase, while the ablation of solid Mg and Fe should transform
into a gas phase that takes more time than gas–gas transformation because of the low velocity
(10 km/s) compared with typical meteors (40 km/s).
4.2. UV-II spectrum in 3000 – 4000 ˚
A
The vibration temperature of molecular N+
2(1) was dramatically changed from 4000 K
at a height of 92.5 km to 13000 K at a height of 82.9 km (table 3; ﬁgure 6). The observed spectra
are a superposition of the post shock plasma radiation which is mixed with a shock layer heating
and downward plasma. Thus, it is logical to understand that the high temperature region was
induced by a shock layer of the HAYABUSA spacecraft which rapidly grew between 92.5 km
and 82.9 km in height. The molecular band of N+
2(1) was also observed in the spectrum of the
Stardust re-entry capsule with a rotational temperature of 15000 K at heights between 71.5 km
and 62 km (Winter & Trumble 2011). Interestingly, at a height of 84 km, N+
2(1) was detected
with a vibration temperature of 10000 K from a –4 magnitude bright ﬁreball of the Leonid
meteor shower whose entry velocity was 72 km/s (Abe et al. 2005b). The ﬂux of the spacecraft
at a height of 62.7 km (–12 absolute magnitude) was about 1600 times brighter than that of
the capsule’s ﬂux (–4 absolute magnitude at the maximum). Therefore, the N+
2(1) bands
originated from the spacecraft was much stronger than CN bands originated from the capsule
in which C was the major erosion product of the Carbon-Phenol heat shield of the capsule as
15
seen by the Stardust capsule (Jenniskens 2010a; Winter & Trumble 2011). Clear C Ilines were
also observed in the near-infrared spectrum (around 1 µm wavelength) of the Stardust reentry
capsule (Taylor & Jenniskens 2010). Note that the vibrational and rotational temperatures of
CN violet bands were measured to be 8000 ±1000 K in the Stardust capsule at a height of 60
km (Jenniskens 2010b). C–N coupling occurs at a higher excited state than a ground state, and
then vibration-rotation temperature approaches to the translational temperature. For instance,
the estimated translation temperature in the shock layer of the capsule was 11000–13000 K.
Hence, the vibration-rotation temperature of 13000 K for N+
2(1) and CN is reasonable.
Bright ﬁreballs sometimes leave a self-luminous long-lasting plasma at altitudes of about
80–90 km that is called ’persistent trains’. It is generally believed that the luminosity of
persistent trains is fueled by reactions involving O3and atomic O, eﬃciently catalyzed by metals
from the freshly ablated meteoroids (e.g., Jenniskens 2000; Abe et al. 2005a). A persistent train
was observed at heights between 92 km and to 82 km for about 3 minutes(Yamamoto et al.
2011). It is reasonable to suppose that suﬃcient metals were supplied by the ablation of the
spacecraft at these heights.
It is important to understand how meteoroids and meteors supply the Earth with space
matter including organics and water (e.g., Abe et al. 2007b). Meteors represent a unique
chemical pathway towards prebiotic compounds on the early Earth and a signiﬁcant fraction of
organic matter is expected to survive. Thus, the investigations of OH(A-X) in the HAYABUSA
spectrum is of particular interest. The most likely mechanism for emitting OH(A-X) band in
the meteor is caused by the dissociation of water or mineral water in the meteoroid. Our
possible detection of OH(A-X) band indicates an Earthly origin caused by the dissociation of
water in the upper atmosphere. However, due to blending with other atomic lines such as Mg I,
Fe I, and Al I, further spectroscopy with higher resolution and sensitivity around 3090 ˚
A will
be needed for further conﬁrmation.
4.3. Gray-body spectrum of the capsule
A continuum consisting of a gray-body emission of the capsule at near-ultraviolet and
visible wavelengths was examined. A continuum radiation of the capsule obtained at a height
of 42 km was that of a gray-body at a ﬁtted temperature employing Planck’s formula. Our
derived temperature from an excellent UV-II data set was 2437 ±14 K at a height of 41.8 km
(ﬁgure 7). The surface temperature of 2525 K ±50 K at a height of 41.1 km was estimated
based on radiative equilibrium Computational Fluid Dynamics (CFD) (Fujita et al. 2003). Our
observed temperature agrees qualitatively with the CFD model prediction. The gray-body
temperature observed from NAOJ’s team at Coober Pedy resulted in 2400 ±300 K at a
height of 40.5 km (Ohnishi et al. 2011) which is comparable with our result. Note that
dynamical pressure at a height around 40 km was the maximum 64 kPa (Yamada & Abe
2006). At the GOS3 site, a strong sequence of sonic booms was detected at 13:55:21 UT using
16
a video recorder’s microphone which was observed at Tarcoola by Y. Akita and his colleagues.
A sonic boom is the sound associated with a shock wave created by the supersonic ﬂight of
the capsule. According to this time delay, the shock wave generation point was estimated at
a height around 40 km. Considering these ﬂuid conditions, further analysis will be made in a
forthcoming paper (e.g., Fujita et al. 2011b).
5. Conclusion
At 13:51:50 UT on June 13, 2010, the HAYABUSA spacecraft appeared as planned in the
dark sky over the Australian desert, along with the faint dot of the capsule. The HAYABUSA
spacecraft was ﬂying behind the capsule, roughly 1 km above as if he must protect his tiger cub.
While the spacecraft burst into many fragments, as if falling into the Milky Way, the capsule
became an independent bright ﬁreball wearing an ablative heat shield as its thermal protection
system (TPS), as if demonstrating its will to overcome adversity. The planned atmospheric
re-entry was perfectly completed. The HAYABUSA spacecraft ended his journey in a brilliant
ﬂash of light that provided us a treasure trove of “artiﬁcial ﬁreball” data, which has never been
observed in a scientiﬁc way. Atomic lines such as Fe I, Mg I, Na I, Al I, Cr I, Mn I, Ni I, Ti I, Li I,
Zn I, O I, and N Iwere identiﬁed. The excitation temperature ranging from 4500 K to 6000 K
was estimated using Fe Iand Mg Iwithin the 5000 – 5500 ˚
A wavelength region, which is similar
to a common excitation temperature of meteors and bolides. The identiﬁcation of emission lines
may be inadequate and contain some unknown lines. Exotic atoms such as CuI, Mo I, Xe I,
and Hg Iwere also identiﬁed. The explosion of the spacecraft injected a large amount of iron
which increased the density of Fe I. The surprising strong red line during the last ﬂash of the
spacecraft was well explained by a Li Iline (6708 ˚
A) that was probably caused by explosions of
the onboard Li-Ion batteries. A clearly detected FeO band at a height of 63 km is similar to
a common bolide spectrum which is likely to emit in the wake, where the radiation is emitted
just behind the body. The alteration in the hot plasma temperature of N+
2(1) bands (from
4000 K to 13000 K) appears to be the strongest proof that an intense shock layer around the
HAYABUSA spacecraft was rapidly formed at heights between 93 km and 83 km. The gray-
body temperatures ranging from 2482 K to 2395 K were measured at heights between 42.7
km and 41.2 km that can be explained by the CFD model prediction. Further investigation
is required to understand the performance of the TPS. Our experiences will be instructive in
observing the planned HAYABUSA-II Earth return mission.
Acknowledgements. We are thankful to all of the ISAS/JAXA personnel who organized
and participated in the recovery operations, especially Jun-ichiro Kawaguchi, Hitoshi Kuninaka,
Tetsuya Yamada, Makoto Yoshikawa, Masanao Abe, and Hajime Yano. We are also grateful
to all of the JAXA ground observation team members at JAXA, NAOJ, Kochi University of
Technology, Kanazawa University, and Nagoya University who assisted in observing at GOS3
17
and GOS4 stations. GOTO Inc. and NEC Corp. kindly provided a newly developed high-
sensitive EMCCD camera (NCR-550a). Noboru Ebizuka (Nagoya University) designed the
UV-II spectroscopic camera with the aid of SHOWA Industry Co., Ltd in Japan. Yuichiro
Akita kindly provided recording data of the sonic boom observed at Tarcoola. We express
many thanks to Jiˇı Boroviˇcka (Ondˇrejov observatory) for constructive comments and kind
advice. Synthetic spectrum was carried out in part on the general-purpose PC farm at the
Center for Computational Astrophysics (CfCA) of NAOJ. Shinsuke Abe is supported by JAXA
and the National Science Council of Taiwan (NSC 97-2112-M-008-014-MY3, NSC 100-2112-M-
008-014-MY2). Welcome Back Home “Okaerinasai” HAYABUSA!
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19
Table 6. Identiﬁcation of atoms and molecules in 4200 – 6800 ˚
A. All atoms except Li Iin the table were analyzed from the
spacecraft spectrum at a height of 62.7 km (13:52:16 UT). Li Ilines resulted from the spacecraft spectrum at a height of 54.9
km (13:52:21 UT). Identiﬁed atoms are indicated in the visual spectrum (ﬁgure 3). The values for intensities were measured
in relative units.
Observed line Identiﬁed line
Wavelength (˚
A) Intensity Wavelength (˚
A) Element multiplet
4234 10.9 4234 Fe I152
4236 11.0 4236 Fe I52
4256 12.2 4254 Cr I1
4262 29.3 4261 Fe I152
4282 24.7 4272 Fe I42
24.7 4275 Cr I1
24.7 4290 Cr I1
4300 19.5 4308 Fe I42
4358 6.1 4358 Hg I1
4388 5.1 4384 Fe I41
4408 2.0 4405 Fe I41
4414 2.0 4415 Fe I41
4434 3.4 ? –
4466 2.8 4467 Fe I350
4502 1.6 ? –
4538 13.8 4533 Ti I42
4558 19.2 ? –
4575 8.6 ? –
4618 1.8 4617 Ti I4
4622 1.6 4624 Xe I1
4656 14.6 4651 Cu I1
4670 10.2 4671 Xe I1
4684 16.0 4680 Zn I1
4704 7.3 4705 Cu I1
4724 4.0 4722 Zn I1
4540 1.7 ? –
4760 2.6 4754 Mn I16
4762 2.2 4762 Mn I21
4782 1.6 4783 Mn I16
4811 3.6 4811 Zn I1
4822 4.3 4824 Mn I16
4846 12.0 ? –
20
Table 6. (Continued.)
Observed line Identiﬁed line
Wavelength (˚
A) Intensity Wavelength (˚
A) Element multiplet
4868 9.3 4861 H I20
4872 9.0 4872 Fe I318
4898 7.0 4891 Fe I318
4912 6.4 ? –
4932 9.2 ? –
4958 4.3 4957 Fe I318
4982 6.1 4982 Ti I38
4992 4.7 4991 Ti I38
5014 6.4 5014 Ti I38
5040 8.6 ? –
5081 5.8 5081 Ni I4
5016 9.4 5106 Cu I1
5125 2.7 ? –
5146 3.2 5147 Ti I1
5170 8.2 5167 Mg I2
8.2 5167 Fe I37
8.2 5173 Mg I2
5184 7.8 5184 Mg I2
5208 7.4 5205 Cr I7
7.4 5205 Fe I1
7.4 5206 Cr I7
7.4 5208 Cr I7
5246 4.6 ? –
5268 10.2 5270 Fe I15
5296 11.3 5293 Cu I1
5326 13.8 5328 Fe I15
13.8 5331 O I12
5344 12.2 ? –
5370 11.1 5371 Fe I15
5378 3.5 5383 Fe I1146
5394 8.5 5393 Fe I553
5397 4.0 5397 Fe I15
5407 12.6 5404 Fe I1165
12.6 5406 Fe I15
5429 10.0 5430 Fe I15
21
Table 6. (Continued.)
Observed line Identiﬁed line
Wavelength (˚
A) Intensity Wavelength (˚
A) Element multiplet
5448 7.6 5447 Fe I15
5460 8.9 5456 Fe I15
8.9 5461 Hg I1
5488 3.6 ? –
5510 6.7 5506 Mo I1
5534 15.5 5533 Mo I1
5702 32.5 5700 Cu I1
5784 39.8 5782 Cu I1
5856 21.0 ? –
5870 4.9 ? –
5896 40.2 5890 Na I1
40.2 5896 Na I1
6104 2.2 6104 Li I2
6152 10.0 6156 O I10
6702 4.7 6708 Li I1
5500-6100 FeO –
22

## Supplementary resource (1)

Data
July 2013
... La première est le temps nécessaire pour accomplir une telle mission. Il s'est en effet écoulé près de 7 ans avant qu'Hayabusa 1 ne rentre sur Terre, New Horizons aura mis 9 ans pour atteindre la ceinture de Kuiper, Voyager 1 a atteint les limites du système solaire en 28 ans et devra encore poursuivre pendant près de 300 ans avant de pénétrer dans le nuage de Oort [53,54]. La seconde limite réside dans le risque inhérent à toute mission spatiale : celui d'un échec de celle-ci, réduisant à néant des années de travail ainsi que les attentes scientifiques qui lui sont liées. ...
Thesis
Les météorites et particules de poussière interplanétaire apportent des contraintes sur la formation et l'évolution de la matière dans le système solaire. Les micrométéorites, dont certaines proviennent des régions externes du système solaire, représentent la source dominante de matière extraterrestre arrivant sur Terre. Les micrométéorites collectées dans les neiges antarctiques sont dans un excellent état de conservation du fait de conditions géographiques et météorologiques favorables à leur préservation. La collection CONCORDIA/CSNSM de micrométéorites contient en particulier des micrométéorites peu altérées thermiquement lors de leur entrée atmosphérique. Certaines sont caractérisées par une très haute teneur en matière organique, dépassant 50% en volume, très largement au dessus des valeurs habituelles trouvées dans les météorites. Cette matière organique présente de plus la spécificité d'être fortement enrichie en deutérium et contient jusqu'à cinq fois plus d'azote celle extraite des météorites.Les différents scénarios proposés pour expliquer la formation de cette matière et satisfaisant à l'ensemble des caractéristiques de ces micrométéorites impliquent des corps parents orbitant au-delà de Neptune, dans la ceinture de Kuiper ou dans le nuage de Oort. La température y est suffisamment basse pour condenser à leur surface les molécules volatiles comme l'azote et le méthane tandis qu'ils sont exposés à l'action radiochimique du rayonnement cosmique galactique. Afin de contraindre ces scénarios, des expériences ont été conduites en exposant différentes glaces N2-CH4 aux faisceaux d'ions du GANIL simulant ce rayonnement. L'évolution chimique des glaces au cours de l'irradiation et pendant le recuit des échantillons a été suivie au moyen de deux dispositifs disponibles au CIMAP : la chambre CASIMIR et le nouvel appareil IGLIAS. Des analyses complémentaires ex situ ont été menées par spectrométrie de masse. Les résultats apportant des éléments de réponse à l'origine de la matière organique des micrométéorites ultracarbonées ainsi que sur l'origine de leur enrichissement isotopique seront présentés et discutés.
... Artificial bodies exhibit different spectra. The Hayabusa spacecraft contained exotic lines of Cu and Mo in the same spectral range (Abe, et al., 2011). The near-UV spectra obtained during the ESA ATV1 reentry show dominance of Al and weakness of Fe (Löhle, Wernitz, Herdrich, Fertig, Röser, & Ritter, 2011). ...
Full-text available
Article
Temporarily Captured Orbiters (TCOs) are Near-Earth Objects (NEOs) which make a few orbits of Earth before returning to heliocentric orbits. Only one TCO has been observed to date, 2006 RH120, captured by Earth for one year before escaping. Detailed modeling predicts capture should occur from the NEO population predominantly through the Sun-Earth L1 and L2 points, with 1% of TCOs impacting Earth and approximately 0.1% of meteoroids being TCOs. Although thousands of meteoroid orbits have been measured, none until now have conclusively exhibited TCO behaviour, largely due to difficulties in measuring initial meteoroid speed with sufficient precision. We report on a precise meteor observation of January 13, 2014 by a new generation of all-sky fireball digital camera systems operated in the Czech Republic as part of the European Fireball Network, providing the lowest natural object entry speed observed in decades long monitoring by networks world-wide. Modeling atmospheric deceleration and fragmentation yields an initial mass of ~5 kg and diameter of 15 cm, with a maximum Earth-relative velocity just over 11.0 km/s. Spectral observations prove its natural origin. Back-integration across observational uncertainties yields a 92 - 98% probability of TCO behaviour, with close lunar dynamical interaction. The capture duration varies across observational uncertainties from 48 days to 5+ years. We also report on two low-speed impacts recorded by US Government sensors, and we examine Prairie Network event PN39078 from 1965 having an extremely low entry speed of 10.9 km/s. In these cases uncertainties in measurement and origin make TCO designation uncertain.
... The Stardust shield was constructed of PICA, a phenolic-impregnated carbon matrix similar in many aspects to the ASTERM material studied here. In-flight measurements of the Hayabusa reentry also showed evidence of sodium, which was attributed to products of the ablating heat shield [48]. ...
Article
Studies of the ultraviolet and visible emission from an atmospheric pressure air plasma and its interaction with two carbon-based ablative materials were performed in an inductively coupled plasma torch. These experiments were conducted at a plate power of 40 kW, which produced an air plasma in local thermodynamic equilibrium with a maximum temperature of approximately 6200K, corresponding to a specific enthalpy of 16.4 MJ/kg. Three techniques were developed to measure the ablator surface temperature. Recession rates and product species profiles were measured for two different materials (ASTERM™; and carbon-bonded carbon fiber) at a plasma velocity of approximately 20 m/s. Measured surface temperatures were in the range of 2100 to 2300 K, and corresponding hot-wall heat fluxes were approximately 1.4 MW/m2. Spatially resolved profiles of the main species detected in the boundary layer were recorded, and they showed evidence of strong coupling between the ablated material and the freestream.
... The Stardust shield was constructed of PICA, a phenolic-impregnated carbon matrix similar in many aspects to the ASTERM material studied here. In-flight measurements of the Hayabusa reentry also showed evidence of sodium, which was attributed to products of the ablating heat shield [48]. ...
Conference Paper
Studies of the UV and visible emission from an atmospheric pressure air plasma in local thermodynamic equilibrium and its interaction with two carbon-based ablative materials were performed in an inductively coupled plasma torch. These experiments were conducted at a plate power of 40 kW, which produced an air plasma of near 6500 K. Recession rates and product species profiles were measured for two different materials (ASTERM and carbon bonded carbon fiber) at two different flow conditions.
... In addition, strong radiative emission is expected to take place, whose characteristics (intensity, spectrum) depend on the spacecraft velocity and the atmospheric composition. Observation campaigns have insofar only been successful for Earth re-entries such as NASA Stardust spacecraft in January 2006 [12], ESA Jules Verne Automated Transfer Vehicle (ATV) in September 2008 [13], and JAXA HAYABUSA spacecraft in June 2010 [14]. The main motivation for such measurement is that, first, it would provide the confirmation of the time of the atmospheric entry. ...
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NASA's PHOENIX spacecraft has successfully landed on Mars on 25 May 2008. ESA supported the event by recording signals from PHOENIX by the Mars EXPRESS spacecraft using its lander communication subsystem. Following numerical simulations of the probe entry plume emission, two Mars EXPRESS instruments, namely the High Resolution and Stereo Camera (HRSC) and the Ultraviolet and Infrared Spectrometer (SPICAM), were switched on in to observe the emission associated with the atmospheric entry. No positive detection was reported unfortunately. This article reports on the simulations, the planning, and the results. The non-detection by the UV spectrometer was due to a wrong instrument setting. Result for the camera is tentatively explained by the level of emission in the visible range. Lessons learned are given in the conclusions: the entry probe trajectory should be communicated as soon as possible to all interested parties, within the boundary conditions of confidentiality obviously. It is important to plan some redundancy to prevent incorrect instrument operations. A multi-instrument multi-spacecraft campaign should be encouraged by all means. Since detection of such faint signal is challenging, the integration time must be properly matched to the event duration. Payload operational (exclusion) rules should be discussed in an open way, to check whether the prudence of such measures is procedural or physical. The numerical simulations discussed in this paper have been focused on IR radiation in the lower density flow wake, using a DSMC/line-by-line method. These could be complemented with other numerical approaches more focused in the VUV-visible region in the high-pressure bow-shock region, using continuum Navier-Stokes fluid methods, which would yield information on the contribution to the emission spectrum from minor flow species such as CN, C2 and C.
Conference Paper
View Video Presentation: https://doi.org/10.2514/6.2022-3420.vid In order to successfully design spacecraft which will be able to return from Mars experimental simulation of the conditions likely to be experienced during the re-entry of Earth’s atmosphere need to be reliable and optimised to credibly inform future spacecraft design. The aim of this study is to identify an optimal condition design metric. The X2 expansion tunnel at The University of Queensland was used to test different shock tube and acceleration tube fill pressure combinations for flow velocities from 12-15 kms−1, which are likely to represent conditions experience during Earth re-entry from Mars return trajectories. The ratio between shock speed in the shock tube and acceleration tube was chosen a suitable metric to base condition design on. It was found that with increasing this ratio the test condition led to an increase in test time and decrease in the standard deviation of pitot pressure throughout the test time. The range of conditions explored suggested there could be an optimal shock speed ratio, above which the quality of the flow condition produced decreases. However, further investigation is needed.
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On 2020 December 5 at 17:28 UTC, the Japan Aerospace Exploration Agency’s Hayabusa-2 sample return capsule came back to the Earth. It re-entered the atmosphere over South Australia, visible for 53 seconds as a fireball from near the Northern Territory border toward Woomera where it landed in the the Woomera military test range. A scientific observation campaign was planned to observe the optical, seismo-acoustic, radio, and high energy particle phenomena associated with the entry of an interplanetary object. A multi-institutional collaboration between Australian and Japanese universities resulted in the deployment of 49 instruments, with a further 13 permanent observation sites. The campaign successfully recorded optical, seismo-acoustic, and spectral data for this event which will allow an in-depth analysis of the effects produced by interplanetary objects impacting the Earth’s atmosphere. This will allow future comparison and insights to be made with natural meteoroid objects.
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Conference Paper
The primary objective of the Hayabusa Re-entry Observing Campaign was to measure time resolved absolute irradiance of radiation emitted by the Hayabusa Sample Return Capsule during the 2010 June 13 reentry over the Woomera Test Range, Australia. The measurements reported here were made from NASA's DC-8 Airborne Laboratory with an array of CCD cameras equipped with transmission gratings. The aircraft was positioned just south of the landing area at the time of entry. The irradiance measurements cover a wide wavelength range from 405 - 890 nm at ∼1 nm full-width-at-half-maximum resolution, and from 950 - 1330 nm at 2.3 nm resolution. The capsule was resolved from the rest of the fragmenting spacecraft over most of its entry trajectory. Results were calibrated against two ground-based radiance calibration lamps at the tarmac in Palmdale, CA, and against background stars Canopus and Vega. Time resolved absolute irradiance is presented averaged over intervals of 1 second, both as observed at the aircraft and corrected to a common distance of 100 km with no atmospheric extinction in the line of sight (and the capsule fore body seen head-on). The data include a temporal evolution of continuum emission, presumably from the hot thermal protection system heat shield surface, air plasma shock emission lines (from excited oxygen and nitrogen atoms), and emission lines from atoms that derive from the heat shield, including aluminum, hydrogen, sodium, calcium, and potassium. This data can now be interpreted to reveal quantities of importance to atmospheric entry aerothermodynamics: apparent temperatures, shock radiation emissions, rate of ablation and their temporal evolution during entry. Such interpretations will be discussed elsewhere. © 2012 by the American Institute of Aeronautics and Astronautics, Inc.
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We performed low-resolution spectroscopic observations of the capsule of the HAYABUSA spacecraft during re-entry into the Earth's atmosphere on 2010 June 13 UT as an artificial meteor. We obtained the photometric magnitude of the HAYABUSA capsule using zeroth-order spectra. The efficiency of the zeroth-order spectra was too low for us to measure the magnitude of the capsule without any saturation at all times. The altitude at the maximal flux of the capsule was at around 56 km (13$^{\rm h}$52$^{\rm m}$19$\!\!\!^{\rm s}$81 UT), which is almost similar to the case GENESIS, i.e., the maximal flux at around 55 km. We examined the change in the spectrum shape of the capsule as a function of its altitude, and investigated the emission from the shock layer and the blackbody radiation from the surface of the capsule. It is found that the shock-layer emission was dominant, and/or on the same order of the blackbody radiation at the early phase of re-entry; also, the emission from blackbody radiation was dominant during the last phase of re-entry. We measured the surface temperature of the capsule along the trajectory; during the last phase before dark flight, we found that the blackbody temperature of the capsule was 3100$\ \pm\$300 K at an altitude of around 50 km, and 2400$\ \pm\$300 K at an altitude of around 40 km.
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Acoustic/infrasonic/seismic waves were observed during the re-entry of the Japanese asteroid explorer HAYABUSA'' at 6 ground sites in Woomera, Australia, on 2010 June 13. Overpressure values of infrasound waves were detected at 3 ground sites in a range from 1.3 Pa, 1.0 Pa, and 0.7 Pa with each distance of 36.9 km, 54.9 km, and 67.8 km, respectively, apart from the SRC trajectory. Seismic waveforms through air-to-ground coupling processes were also detected at 6 sites, showing a one-to-one correspondence to infrasound waves at all simultaneous observation sites. Audible sound up to 1 kHz was recorded at one site with a distance of 67.8 km. The mother spacecraft was fragmented from 75 km down to 38 km with a few explosive enhancements of emissions. A persistent train of HAYABUSA re-entry was confirmed at an altitude range of between 92 km down to 82 km for about 3 minutes. Light curves of 136 fragmented parts of the spacecraft were analyzed in detail based on video observations taken at multiple ground sites, being classified into three types of fragmentations, i.e., melting, explosive, and re-fragmented types. In a comparison between infrasonic waves and video-image analyses, regarding the generation of sonic-boom type shock waves by hypersonically moving artificial meteors, both the sample return capsule and fragmented parts of the mother spacecraft, at an altitude of 40 ± 1 km were confirmed with a one-to-one correspondence with each other.
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The HAYABUSA spacecraft re-entered the Earth's atmosphere on 2010 June 13 UT, together with the capsule for the sample return. This was the first trial of the re-entry experiment as a Japanese interplanetary spacecraft. We undertook an expedition to South Australia for ground-based observations, and succeeded in obtaining valuable data of various phenomena occurring at this re-entry. Our data were widely used not only for scientific analysis, but also for outreach purposes. This paper provides an overview of our expedition.
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Thermal radiation of the heatshield and the emission of the postshock layer around the Stardust capsule, during its reentry, were detected by a NASA-led observation campaign aboard NASA's DC-8 airborne observatory involving teams from several nations. The German sur experiment used a conventional spectrometer, in a Czerny-Turner configuration (300 mm focal length and a 600 lines/mm grating), fed by fiber optics, to cover a wavelength range from 324 to 456 nm with a pixel resolution of 0.08 nm. The reentering spacecraft was tracked manually using a camera with a view angle of 20 deg, and light from the capsule was collected using a small mirror telescope with a view angle of only 0.45 deg. Data were gathered with a measurement frequency of 5 Hz in a 30-s time interval around the point of maximum heating until the capsule left the field of view. The emission of carbon nitride (as a major ablation product), N(2)(+) and different atoms were monitored successfully during that time. Because of the nature of the experimental setup, spatial resolution of the radiation field was not possible. Therefore, all measured values represent an integration of radiation from the visible part of the glowing heatshield, and from the plasma in the postshock region. Further, due to challenges in tracking, not every spectrum gathered contained data. The measured spectra can be split up into two parts: 1) continuum spectra, which represent a superposition of the heatshield radiation and the continuum radiation of particles due to microspallation in the plasma, and 2) line spectra from the plasma in the shock layer. Planck temperatures (interpreted as the surface temperatures of the Stardust heatshield) were determined assuming either a constant surface temperature, or a temperature distribution deduced from numerical simulation. The constant surface temperatures are in good agreement with numerical simulations, but the peak values at the stagnation point are significantly lower than those in the numerical simulation if a temperature distribution over the surface is assumed. Emission bands of carbon nitride and N(2)(+) were tracked along the visible trajectory and compared with a spectral simulation with satisfying agreement. Values for the integrated radiation of the transitions of interest for these species were extracted from this comparison.
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2=nm=sr. Absolute calibration errors add to these values a systematic uncertainty of about 20%. The capsule’s heat shield consistedofaphenol-impregnatedcarbonablator.Hence,theintensityofthecarbon-atomlineemissionisameasure oftheablationrateduringdescent,butitalsodependsonthedetailsofcarbon-atomablationandtheexcitationinthe shock layer.
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During the 2006 Stardust Sample Return Capsule entry observing campaign, the highest spectral resolution data gathered onboard NASA's DC-8 Airborne Laboratory was measured with a fixed-mounted slitless cooled charge. coupled-device spectrograph, called ASTRO. Spectra were recorded around the time of peak heating similar to 09 : 57 : 33 Coordinated Universal Time (UTC) on 15 January. The data covered three 0.8-second time intervals centered on 09:57:32.5, 34.4 and 36.3 s (+/- 0.5 s) UTC, when the capsule was at an altitude of 60 and 210 km from the spectrometer. The observed spectrum was a composite of first-, second-, and third-order emissions. The first-order spectrum contained only continuum emission. Second-order emissions included the 615 nm atomic line of oxygen: third-order emissions included the CN violet 0-0 band, the isoelectric N(2)(+) band, and two Ca(+) atomic lines. The Ca(+) lines had an instrumental full-width at half-maximum of 0.15 +/- 0.01 nm. The CN violet band contour measured vibrational and rotational excitation temperatures of T(v) = T(r) = 8, 000 +/- 1, 000 K, if self-absorption is neglected.
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An unidentified pseudo-continuum in the 600 nm region is observed in the upper mesosphere with the limb-scanning OSIRIS imaging spectrograph on-board the Odin spacecraft. Averages of low latitude spectra at a series of tangent limb altitudes from 75 to 105 km are assembled and matched with synthetic spectra of the known night airglow emission band systems to isolate the underlying airglow continuum. The upper limit of the NO + O --> NO2* air afterglow continuum component in the observed 600 nm pseudo-continuum is estimated to be 5% at low latitudes. The spectral profile of the unidentified 600 nm residual airglow continuum is very similar to published laboratory measurements of the `orange bands' of FeO. The volume emission rate altitude profile of this 600 nm airglow continuum, derived from averaged limb radiance profiles, is very similar in shape and in altitude to the concurrently observed Na vertical profile suggesting related source mechanisms.
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Spectroscopic observations of the 2006 Stardust Sample Return Capsule entry are presented, obtained by means of a slitless miniature echelle spectrograph onboard NASA's DC-8 airborne laboratory. The data cover the wavelength range from 336 to 880 nm, at 0.14-0.9 nm resolution, and were obtained during the time interval when radiative heating was most important. The data contain a broadband continuum, presumably from the hot heat-shield surface, shock-layer air plasma emissions of N, O, and N(2)(+), and atomic hydrogen and CN molecular band emission from the ablating heat-shield material, a form of phenol-impregnated carbon ablator. Early in flight, there were also atomic line emissions of Zn, K, Ca(+), and Na, presumably from a white Z-93P paint applied to the top of the phenol-impregnated carbon ablator. At each moment along the trajectory, the whole spectrum was recorded simultaneously, but broken into smaller segments. Key issues addressed in the data reduction and calibration are described. The interpretation of these data was given elsewhere.
Forebody and aftbody radiative heating rates of the MUSES-C asteroid sample return capsule have been assessed along the reentry trajectory from an engineering standpoint. Nonequilibrium hypersonic flows around the capsule with ablation of the thermal protection system involved were determined by CFD calculations, while the radiative heat transfer was computed by the radiation code SPRADIAN in a non-coupled manner with the flow analysis. In order to take into account much uncertainty in the thermal relaxation, chemical reaction, and ablation models used in the flow analysis, parametric studies were performed by changing these models to obtain the conservative estimation of the radiative environments. The radiative heat flux was found to be considerably affected by the ablation model, especially in the aftbody region of the capsule.