Geoscience Reference
In-Depth Information
Table 1. Some properties of the Karin family asteroids.
P
is rotation period (hour),
δM
is peak-to-peak variation magnitude, and
α
is the solar phase angle (degree). Lightcurves
of all asteroids are shown in Figs. 1 and 2. For (832) Karin and (28271) 1999CK16, we
had two opportunities to observe their lightcurves: 2003 and 2004 for (832) Karin, 2002
and 2004 for (28271) 1999CK16.
Asteroid
P
δM
α
Figure #
(832) Karin (2003)
18
.
35
±
0
.
02
0
.
61
±
0
.
02
1-14
1(a)
(832) Karin (2004)
18
.
35
±
0
.
02
0
.
61
±
0
.
01
21.7
1(b)
(28271) 1999CK16 (2002)
5
.
64
±
0
.
06
0
.
08
±
0
.
04
3.1
1(c)
(28271) 1999CK16 (2004)
5
.
64
±
0
.
03
0
.
21
±
0
.
02
8.4
1(d)
(4507) 1990FV
6
.
58
±
0
.
04
0
.
49
±
0
.
03
7.9
1(e)
(16706) Svojsik
6
.
72
±
0
.
07
∼
0.3
12.7
1(f)
(10783) 1991RB9
7
.
33
±
0
.
04
0
.
50
±
0
.
02
5.6
1(g)
(40912) 1999TR171
7
.
81
±
0
.
08
0
.
35
±
0
.
02
1.5
1(h)
(69880) 1998SQ81
9
.
14
±
0
.
01
0
.
08
±
0
.
01
5.3
2(a)
(13765) Nansmith
10
.
51
±
0
.
01
0
.
09
±
0
.
02
11.3
2(b)
(11728) Einer
13
.
62
±
0
.
05
0
.
19
±
0
.
01
10.3
2(c)
(71031) 1999XE68
20
.
19
±
0
.
41
0
.
45
±
0
.
04
5.0
2(d)
(7719) 1997GT36
29
.
56
±
0
.
60
0
.
50
±
0
.
02
18.6
2(e)
(43032) 1999VR26
32
.
51
±
0
.
04
1
.
00
±
0
.
06
10.6
2(f)
Table 2. Major parameters during our multi-color observations of (832) Karin. From
the left, UT referring to the mid-time of each night, distances (AU) between the asteroid
and the Sun (
r
) and the Earth (∆), the ecliptic longitude (
λ
) and latitude (
β
), and the
solar phase angle (
α
) of this asteroid. The unit of angles is degree.
Date (UT)
r
∆
λ
β
α
20030926.19
2.666
1.803
324.8
1.5
13.36
20030927.19
2.666
1.811
324.7
1.5
13.68
20030928.17
2.665
1.819
324.6
1.5
13.99
20030929.17
2.665
1.827
334.5
1.5
14.30
20040922.44
2.706
2.442
63.8
0.2
21.71
20040923.44
2.707
2.429
64.1
0.2
21.68
20040924.45
2.707
2.417
64.3
0.2
21.64
for the lightcurve observation that we described in the previous section, we
performed the multi-color observing sequence several times with intervals
of a few hours. Since we were able to observe this asteroid for 4-5 h every
night, we repeated this procedure seven times in our 2003 observation and
ten times in our 2004 observation. As a result, we obtained color differences
such as
V
-
I
or
B
-
V
. We calculated the errors of these values from the pho-
tometry error of each of the
B
,
V
,
R
,and
I
images: For example, the error
of
V
-
I
is
√
δV
2
+
δR
2
,where
δV
and
δR
are the photometry errors of the
V
and
R
images.
