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/01&'

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B.L. Kashcheyev, S.V. Kolomiyets, “Interstellar particle detection andselection criteria of meteor streams”, Proceedings of the Meteoroids
2001 Conference, ESA SP-495, 643 - 650, 2001

•

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D.D. Meisel, D. Janches, J.D.Mathews, “Extrasolar Micrometeors Radiatingfrom the Vicinity of the Local Interstellar Bubble”, ApJ, 567, 323-341, 2002.

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2*10 *10/10 /10 *0.68/10 =1.4*10 Ó/[•••(3-1)%hi_xC5LY“dzB9o–x•qäÈåMævÐÑ%-3.5 Œ%çè,z%ØÙ|kn{Fp5B•-6-6dBÐÑ 1.7mm,5*10 kg 5%hi,×_|D•dB 10 kg5%†’6T
32
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2*10 /10/10 *0.68/10 =1.4*10 Ó/[•••(4-1)-6%hi_xC5LY“dzB9o–x•qäÈåMævÐÑ%-3.5 Œ%çèB•dBÐÑ 4.6mm,10 kg 5
%hi%†’6T43
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Ñ 112 km5v 1 úÒcG–9ÜÝ•dû÷üýÄ6T
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G–%ÈAý6T´œFµMi¸¢¶·¶tµÀT^É>‘ÄÀ% ¡B—É•ÊFx•q• TNew Zealand%(A¦[4]96TpSµ,Ë: 260Ì, Í: 0Ì5fg9ÈAý_”L“TpSµÀ¢žŸ‚ƒ ¡9o–x•qGwFTÎ %(A¦96Tœ´µfgÚ"%ÏÃ_”L“xœZq: 8ú‘e6ÐÑ¢Ò(¶„%N1OP9-®S!"#$vÓºGŽ [5, 6]6k¬c–xœZ_TMNOP9-d=¥¦§^%Ôêmo(A¦_ÕL“d-œ9odBTy%&'9~pS%Ö×_¡Kßc_®S¬dzBeF7œq

Ø_ ¿Ä[1] ()* +, ;Y ÙÚ, ‚Û ÜÝ,:“IJ!"KL%#$%MNOP”, Þ120<#$=3>?@A®ß,(2008)[2] http://www.geo.titech.ac.jp/lab/ida/STUDIES/basic_process.html[3] B.L. Kashcheyev, S.V. Kolomiyets, “Interstellar particle Detection and Selection Criteria of Meteor Streams”, Proc.
the Meteoroids 2001 Conference, ESA SP-495, 643 - 650, (2001).
[4] Baggaley, W. Jack, “Advanced Meteor Orbit Radar observations of interstellar meteoroids”, JGR, 105,
10353-10362, (2000)[5] R.L. Hawkes, S.C. Woodworth, “Optical detection of two meteoroids from interstellar space”, J. R.
Astron. Soc. Can., 91, 218, (1997)[6] S.C. Woodworth, R.L. Hawkes, “Optical Search for High Meteors in Hyperbolic Orbits”, ASP Conf. Ser.,
104, 83, (1996)

AMOR, 45<Vh<60 (1995-1998)
S2 Khariv9´»d1<e<1.1%ÎàŸàá%#$%—˜ ¡Mæ,áB‚â5[3]q
New Zealand9´»dVƒ…k45-60 km/s%#$%—˜ ¡Mæ,ã5[4]q

!"#$%&'()*+,
Extra-Solar Meteor

GCOE!"#$%&'()*+,-./0 3, Spetember, 2009-./ 0 (123456789:;<=>?@A)
EBIZUKA, Noboru(Plasma Nanotechnology Research Center, Nagoya Univ.)

BC DE (+,FG>H8A)
SHIGENO, Yoshihiko(Meteor Science Seminar)

Detection of interstellar media in the solar system
Particle counter

Ulysses

Arecibo Observatory

Rader© NASA

Galileo

Particle with 10-19~10-11kg (Radius: 0.005~2 !m@1g/cm3) aredetected by particle counters of spacecrafts.
3~30% of particles at 1au are assumed to be interstellar media.
[M. Baguhl et.al. 1996]

Optical

AMOR: University of Canterbury• 10-14~10-9kg (R: 0.2~10 !m@1g/cm3), 4.8% (143/3000)
I e >1.0 (Arecibo, Puerto Rico, D=300m, 430MHz).
• 5x10-9 ~10-6kg (R: 10~100 !m@1g/cm3), 3.2% (7,911/250,000 ) IJe >1.0 (MARS: Ukraine, 31.1MHz).
• >10-10kg (R: >5 !m@1g/cm3), 0.46% (1,600/350,000)
IJVe > 100 km/s (e >2.5, AMOR, New Zealand).

Meteor camera
http://www.ne.jp/asahi/meteor/star/index.html

Super Schmidt cameraKSmithsonian
Astronomical observatory, 1950s eraL

10-4~10-1 kg (R: 0.5~ 5 mm@1g/cm3, Mag.: -3~ -10) : 1.3%
(59/4,581, IAU/MDC Photograph),10-9~10-4 kg (R: 10~500 !m@1g/cm3, Mag.: 9.5~ -3) :1~2%(2/160, Video@Canada) IJe>1.45 (Ve > 46.6 km/s).
e STD: ~ 0.1

Optical meteor observations of Mr. Shigeno• Photograph in 1983, 1987, 1989 and 1991
• I.I. Video camera from 1992 to 2009.
• 3787 trajectory data of meteors.
• Data could download fromhttp://www004.upp.so-net.ne.jp/msswg/ .

Visible mag.

Flux of interstellar particles[M. Hajduková Jr., et.al. (2006)]

Vh

L abs !"#$%&%'()*&+,-.'.#/0%"#$.%'(

1 1.012 1.909 146.4 181.6 177.9 80.0 50.5

3.6 1/2#'/3*--"'4$5#0/.'/64.7"(81

2 0.822 1.382 211.5 225.5 118.7 65.4 46.9

3.4 9/:;(

1

3 0.882 1.244

0.9 9/*(.

No.

Gem Aqr #Eccentricity vs. inclination of meteors

N meteors: 110
e min.: 0.742
e average: 0.908 e max. : 1.056
e STD of Leonid: 0.051

q

e

i

54.2

Ve

36.4 134.5 68.7 45.2

4 0.979 1.208 140.1 200.2 143.0 69.5 44.0

4.6 9/*7"

5 0.916 1.180-0.7 </!&$

54.7 329.8 153.3 71.9 44.3

6 0.926 1.160 32.9 211.5 82.2 49.7
7 0.964 1.146 140.3 155.3 116.4 62.1 43.4

Intersection
angle of images

Aqr $, Ori

Radiant points of Leonid@18, Nov., 2001.
R.A. " Dec. : 2° " 1°3722 meteors (~20, May.,2007) were investigated.
Candidates of extra solar meteors

1

2.9 9/:4&
3.8 </2#'/3*--"'4$5#0/.'/=7-%.#"8 Intersection angle of images of a meteor
trajectory projected on the celestial sphere.
Gem

Per

Leo
Cas
#Aqr

⦿
%&'(

Qua

CVn

Aur
Leo
Ori

q: 1.012
e: 1.909!: 146.4": 146.4
i : 177.9
Asymptote direction: Leo
Approached 5 au to Saturnq: 0.822
e: 1.382!: 211.5": 225.5
i : 118.7
Asymptote direction: Cvn

UV-HDTV camera

UV-HDTV camera (UV sensitive I.I. HDTV camera, above) and I.I.-HDTV
camera with grism (Direct vision
grating, below).

q: 0.882
e: 1.244!: 54.2": 36.4
i : 134.5
Asymptote direction: Ant

q: 0.964
e: 1.146!: 140.3": 155.3
i : 116.4
Asymptote direction: Leo
Approached 2 au to Jupiter

$Aqr

!"#$

Ant

Stereoscopic and spectroscopic observation system for extra-solar meteors

UFOCapture, http://sonotaco.com/• I.I.-HDTV camera is sensitive about 1 magnitude
fainter than a I.I.-CCTV camera since a HDTV camera
have 6 times pixels as a CCTV camera.
• 3 sets of I.I. HDTV cameras will be placed with 20~
50 km in distance.
• Remote observations and automatic detection.
• ~240,000 (150 meteors x 8 hours x 200 nights) of
meteors brighter than 8 magnitude will be detectable
in a year?
• I.I. HDTV camera: ~$15,000/camera
Initial costs: $100,000 ~ $200,000?
Maintenance costs: ~ $20,000?
Human resouce: 2 IJ0.5 persons?
Telescope Array for observations of extreme hight energy cosmic
ray. (Institute for Cosmic Ray Research, Univ. Tokyo, Utah, USA)

Conclusions

UV spectrum of a meteor taken by the UVHDTV camera above and an objective
spectrometer of reflection grating.

Psc

Meteor spectra taken automatically by a grism, CCTV
camera and UFOCaptur. (Dr. K. Maeda, Mikyazaki Univ.)• 0.99% (37/3722) of meteors on Sigeno’s observations are e>1.1.
• Trajectory of 2 meteors have been influenced by Jupiter or Saturn,nevertheless, 5 meteors (0.13%) are supposed to be extra-solar meteor,
among the 7 candidate meteors.
• Several 100,000 of meteors (< 8 mag.) will be detectable in a year bystereoscopic observations with I.I.-HDTV camea.
• Spectral observations for meteors with hyperbolic trajectory provide
direct information of abundance of extra-solar systems.

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