[meteorite-list] x-Boötis (Quadrantids) Meteor Shower

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From: MexicoDoug_at_aol.com <MexicoDoug_at_meteoritecentral.com>
Date: Thu Apr 22 10:18:02 2004
Message-ID: <1e7.160d4df1.2d17b3c7_at_aol.com>

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Ron, =A1=A1 Boo !! as in as in Bootes (formerly somewhat known as Quadrans=20
Muralis), not to pronounce like the "oo" of booties. The latest news on the=
=20
Quadrantids' meteor shower radiating from Bootes. Sounds like there may hav=
e been=20
some major booty shaking and perhaps disintegration of the parent body 2003=20=
EH=20
1. I can't resist asking if anyone can correlate any Jan 3 or (Jan 4?) fall=
s,=20
or there about. This should be a fresh research question. Anne from=20
Impactika.com has listed the following falls for that date:

Jan 2 (none)

Jan 3
1877 Warrenton
1903 St. Mark's=20
1970 Lost City

Jan 4, 5 (none)

Saludos
Doug Dawn
Mexico

http://leonid.arc.nasa.gov/IAUCircular2003Dec8.txt

2003 EH_1 AND THE QUADRANTIDS
P. Jenniskens, NASA Ames Research Center, has pointed out that
2003 EH_1 (cf. MPEC 2003-E27) would seem to be a very strong
candidate for the parent of the Quadrantid meteor stream. The
later orbits, from arcs of up to 48 days (MPO 48330), indicate that
frequent approaches within 0.2-0.3 AU of Jupiter occur, those
during the past century or two evidently increasing q from just
under 1 AU (with other orbital elements also very similar to those
of the Quadrantids) to the present 1.19 AU. The current
theoretical radiant for 2003 EH_1 (R.A. =3D 229.9 deg, Decl. =3D +49.6
deg; V_inf =3D 41.7 km/s at solar longitude 282.94 deg, equinox
2000.0) is at the center of the Quadrantid radiants measured by
photographic means, the narrow dispersion implying a young (about
500 years) shower age. From that dispersion, Jenniskens et al.
(1997, Astron. Astrophys. 327, 1242) suspected that the parent was
still among the meteoroids, hiding as a minor planet. On computing
a parabolic orbit for C/1490 Y1, Hasegawa (1979, Publ. Astron. Soc.
Japan 31, 257) introduced that comet as the likely Quadrantid
parent. In attempting to link the 2003 observations to those of
1490-1491, Jenniskens, and also B. G. Marsden (Center for
Astrophysics), have found that most of the potential solutions with
the required Jan. 1491 perihelion date yield 0.5 < q < 0.6 AU in
1491, and this is probably too small to fit the data used by
Hasegawa. Values in the more acceptable range of 0.7 < q < 0.8 AU
(and 0.80 > e > 0.75) certainly arise for 1488 < T < 1494, however,
the desired date being clearly attainable with the help also of a
close approach to the earth or -- more likely -- the presence of
nongravitational forces. Further light could be shed on the
problem by the recognition of precovery and/or recovery
observations of 2003 EH_1, which is presumably a comet and that
should in any case be considered a high-priority object for further
study.

(C) Copyright 2003 CBAT
2003 December 8 (8252) Daniel W. E. Green

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<HTML><HTML>Ron, =A1=A1 Boo !! as in as in Boot=
es (formerly somewhat known as Quadrans Muralis), not to pronounce like the=20=
"oo" of booties.  The latest news on the Quadrantids' meteor shower rad=
iating from Bootes.  Sounds like there may have been some major booty s=
haking and perhaps disintegration of the parent body 2003 EH 1.  I can'=
t resist asking if anyone can correlate any Jan 3 or (Jan 4?) falls, or ther=
e about.  This should be a fresh research question.  Anne from Imp=
actika.com has listed the following falls for that date: 
 
Jan 2 (none) 
 
Jan 3 
1877 Warrenton 
1903 St. Mark's 
1970 Lost City 
 
Jan 4, 5 (none) 
 
Saludos 
Doug Dawn 
Mexico 
 
 
 
 
http://leonid.arc.nasa.gov/IAUCircular2003Dec8.txt 
 
 
2003 EH_1 AND THE QUADRANTIDS 
     P. Jenniskens, NASA Ames Research Center, has point=
ed out that 
2003 EH_1 (cf. MPEC 2003-E27) would seem to be a very strong 
candidate for the parent of the Quadrantid meteor stream.  The 
later orbits, from arcs of up to 48 days (MPO 48330), indicate that 
frequent approaches within 0.2-0.3 AU of Jupiter occur, those 
during the past century or two evidently increasing q from just 
under 1 AU (with other orbital elements also very similar to those 
of the Quadrantids) to the present 1.19 AU.  The current 
theoretical radiant for 2003 EH_1 (R.A. =3D 229.9 deg, Decl. =3D +49.6 
deg; V_inf =3D 41.7 km/s at solar longitude 282.94 deg, equinox 
2000.0) is at the center of the Quadrantid radiants measured by 
photographic means, the narrow dispersion implying a young (about 
500 years) shower age.  From that dispersion, Jenniskens et al. 
(1997, Astron. Astrophys. 327, 1242) suspected that the parent was 
still among the meteoroids, hiding as a minor planet.  On computing 
a parabolic orbit for C/1490 Y1, Hasegawa (1979, Publ. Astron. Soc. 
Japan 31, 257) introduced that comet as the likely Quadrantid 
parent.  In attempting to link the 2003 observations to those of 
1490-1491, Jenniskens, and also B. G. Marsden (Center for 
Astrophysics), have found that most of the potential solutions with 
the required Jan. 1491 perihelion date yield 0.5 < q < 0.6 AU in 
1491, and this is probably too small to fit the data used by 
Hasegawa.  Values in the more acceptable range of 0.7 < q < 0.8 A=
U 
(and 0.80 > e > 0.75) certainly arise for 1488 < T < 1494, howev=
er, 
the desired date being clearly attainable with the help also of a 
close approach to the earth or -- more likely -- the presence of 
nongravitational forces.  Further light could be shed on the 
problem by the recognition of precovery and/or recovery 
observations of 2003 EH_1, which is presumably a comet and that 
should in any case be considered a high-priority object for further 
study. 
 
            &nbs=
p;         (C) Copyright 2003 CBAT<B=
R>
2003 December 8          &=
nbsp;     (8252)      &nbs=
p;     Daniel W. E. Green 
</HTML>
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Received on Sun 21 Dec 2003 09:41:11 PM PST

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