J/MNRAS/472/4634 Large perihelion dist. Oort spike comets (Krolikowska+, 2017)
Oort spike comets with large perihelion distances.
Krolikowska M., Dybczynski P.A.
<Mon. Not. R. Astron. Soc. 472, 4634 (2017)>
=2017MNRAS.472.4634K 2017MNRAS.472.4634K (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Comets
Keywords: celestial mechanics - comets: general - Oort Cloud
Abstract:
The complete sample of large-perihelion nearly-parabolic comets
discovered during the period 1901-2010 is studied, starting with
their orbit determination. Next, an orbital evolution that includes
three perihelion passages (previous-observed-next) is investigated
in which a full model of Galactic perturbations and perturbations from
passing stars is incorporated. We show that the distribution of
planetary perturbations suffered by actual large-perihelion comets
during their passage through the Solar system has a deep, unexpected
minimum around zero, which indicates a lack of 'almost unperturbed'
comets. Using a series of simulations we show that this deep well is
moderately resistant to some diffusion of the orbital elements of the
analysed comets. It seems reasonable to assert that the observed
stream of these large perihelion comets experienced a series of
specific planetary configurations when passing through the planetary
zone. An analysis of the past dynamics of these comets clearly shows
that dynamically new comets can appear only when their original
semimajor axes are greater than 20000au. On the other hand,
dynamically old comets are completely absent for semimajor axes longer
than 40000au. We demonstrate that the observed
1/aori-distribution exhibits a local minimum separating dynamically
new from dynamically old comets. Long-term dynamical studies reveal a
wide variety of orbital behaviour. Several interesting examples of the
action of passing stars are also described, in particular the impact
of Gliese 710, which will pass close to the Sun in the future.
However, none of the obtained stellar perturbations is sufficient to
change the dynamical status of the analysed comets.
Description:
We constructed a sample of near-parabolic comets with q>3.1au and
1/aori<0.000200au-1; that is, large-perihelion comets with
original semimajor axes larger than 5000au. The majority of comets
satisfying both conditions (74 objects) were taken from Krolikowska
(2014, Cat. J/A+A/567/A126) and Krolikowska et al. (2014, Cat.
J/A+A/571/A63). However, for five of these 74 comets we decided to
repeat an orbit determination because the previous orbits were based
on a shorter arc of observations and, in addition, we found NG effects
in the motion of two of them. To complete the sample of
large-perihelion comets with original semimajor axes greater than
5000au, we analysed 26 more comets discovered since 1950 and
previously not considered by us. As a result, we present new orbital
solutions for 31 LPCs.
Our final sample therefore consists of 100 large-perihelion comets
having 1/aori less than 2x10-4au-1 and represents the complete
sample of all such objects discovered in the years 1901-2010
(94 comets); in addition six more comets detected after 2010 are
included. Note that in the years 1901-1960 only nine large-perihelion
comets were discovered, while as many as 45 comets were detected in
the period 2001-2010.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 177 101 Description of observational material and the new
orbital quality assessment for 100
near-parabolic comets
tableb1.dat 175 101 *Heliocentric orbital elements of osculating
orbits for 100 comets given in Table A1
tablec1.dat 175 101 *Barycentric orbital elements of original orbits,
for 100 near-parabolic comets given in Table A1
tabled1.dat 175 100 Barycentric orbital elements of future orbits,
for 100 near-parabolic comets given in Table A1
tablee3.dat 186 100 Barycentric orbital elements at previous
perihelion
tablef3.dat 186 100 Barycentric orbital elements at next perihelion
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Note on tableb1.dat and tablec1.dat: for the comet C/2003 WT42 there are two
records with two different solutions.
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See also:
J/A+A/567/A126 : Warsaw Catalogue of cometary orbits (Krolikowska, 2014)
J/A+A/571/A63 : New catalogue of one-apparition comets (Krolikowska+, 2014)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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2- 13 A12 --- Desig Comet's designation
15- 38 A24 --- Cname Comet's designation
39- 44 F6.3 AU qosc Osculating perihelion distance
51- 58 I8 "YYYYMMDD" T Perihelion date, [TT] (G1)
65- 72 I8 "YYYYMMDD" arc1 Date of the first observation, [TT] (G1)
75- 82 I8 "YYYYMMDD" arc2 Date of the last observation, [TT] (G1)
87- 91 I5 --- Nobs Number of observations taken into account
96-100 F5.2 yr arcY Interval of data (arc in years)
105-109 F5.2 AU dh1 Heliocentric distance of the first observation
111-115 F5.2 AU dh2 Heliocentric distance of the last observation
121-129 A9 --- Data Data type in the sense of time-distribution
131-135 A5 --- Model Model type (gravitational or non-gravitational)
139-141 F3.1 --- Q*GR Accuracy of gravitational orbit
147-149 F3.1 --- Q*NG ? Accuracy of non-gravitational orbit when
determinable
155-157 A3 --- Qlnew New quality orbit assessment
162-165 F4.2 arcsec rms Root-mean-square error
167-171 I5 --- Res Number of residuals taken for orbit
determination for a given model
176-177 A2 --- Ref References to the solution (G2)
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Byte-by-byte Description of file: tableb1.dat tablec1.dat tabled1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Desig Comet's designation
14- 21 I8 "YYYYMMDD" Epoch Epoch of osculation (G1)
24- 42 A19 "Y-M-D" T Perihelion time, [TT] YYYY-MM-DD.dddddddd (G1)
44- 53 F10.8 d e_T Uncertainty of Perihelion time in days
55- 65 F11.8 AU q Perihelion distance
67- 76 F10.8 AU e_q Uncertainty of perihelion distance
78- 87 F10.8 --- e Eccentricity
89- 98 F10.8 --- e_e Uncertainty of eccentricity
100-109 F10.6 deg Arg Argument of perihelion, ω (J2000)
111-118 F8.6 deg e_Arg Uncertainty of argument of perihelion (J2000)
120-129 F10.6 deg Long Longitude of the ascending node,
{OMEGA} (J2000)
131-138 F8.6 deg e_Long Uncertainty of longitude of the ascending node
140-149 F10.6 deg i Inclination (J2000)
151-158 F8.6 deg e_i Uncertainty of inclination (J2000)
160-168 F9.2 10-6AU-1 1/a Inverse of semimajor axis (1/aosc)
(J2000)
170-175 F6.2 10-6AU-1 e_1/a Inverse of semimajor axis
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Byte-by-byte Description of file: tablee3.dat tablef3.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Desig Comet's designation
15- 18 I4 --- R Number of returning VCs in the swarm
20 A1 --- n_R [*] '*' means nominal solution is among
returning part of swarm
23- 26 I4 --- E Number of escaping VCs in the swarm
28 A1 --- n_E [*] '*' means nominal solution is among
escaping part of swarm
31- 34 I4 --- H Number of hyperbolas among escaping VCs in
the swarm
36 A1 --- n_H [*] '*' means nominal solution is among
hyperbolic part of swarm
39- 47 F9.2 10-6AU-1 1/a1-10 Inverse of the semimajor axis
(1/aprev or 1/a_next)):
first decile or mean value
(in 10-6AU-1 unit) (G3)
49- 55 F7.2 10-6AU-1 1/a1-50 Inverse od the semimajor axis:
median or standard deviation
(in 10-6AU-1 unit)(G3)
59- 64 F6.2 10-6AU-1 1/a1-90 ? Inverse of the semimajor axis:
third decile (in 10-6AU-1 unit) (G3)
67 A1 ---- 1/a1R [R] 'R' means that the result for the inverse
of the semimajor axis is for a returning part
of the swarm only
70- 79 F10.6 au q10 Perihelion distance (qprev or qnext):
first decile or mean value (G3)
81- 90 F10.6 au q50 Perihelion distance: median or standard
deviation (G3)
92-100 F9.4 au q90 ? Perihelion distance:: third decile (G3)
103 A1 ---- qR [R] 'R' means that the result for the
perihelion distance is for a returning part
of the swarm only
106-113 F8.4 1000au Q10 ? Aphelion distance (Qprev or Qnext):
first decile or mean value (G3)
116-123 F8.4 1000au Q50 ? Aphelion distance:
median or standard deviation (G3)
126-132 F7.2 1000au Q90 ? Aphelion distance: third decile (G3)
134 A1 ---- QR [R] 'R' means that the result for the aphelion
distance is for a returning part of the
swarm only.
137-145 F9.6 Myr t10 Time interval to previous perihelion
(Timeprev or Timenext):
first decile or mean value (G3)
148-156 F9.6 Myr t50 Time interval to previous perihelion:
median or standard deviation (G3) (1)
159-164 F6.3 Myr t90 ? Time interval to previous perihelion:
third decile (G3)
166 A1 ---- tR [R] 'R' means that the result for the time
interval is for a returning part of the
swarm only
169-171 I3 % p1 ? Percentage of VCs with q<10
174-176 I3 % p2 ? Percentage of VCs with 10<q<20
179-181 I3 % p3 ? Percentage of VCs with q>20
184-186 A3 --- Stat Code for the dynamical status (2)
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Note (1): if t50 equals 0.0 it means that the whole swarm was stopped
synchronously and all time intervals are equal.
Note (2): For a dynamical status we use following codes:
DO = most probably dynamically old
DO+ = definitely dynamically old
DN = most probably dynamically new
DN+ = definitely dynamically new
DU = dynamical status is uncertain
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Global notes:
Note (G1): dates are in the format of YYYYMMDD, where the month is coded as:
January - 01, February - 02, ... , December - 12.
Note (G2): references are coded as follows:
P1 = Krolikowska and Dybczynski, 2010MNRAS.404.1886K 2010MNRAS.404.1886K
P2 = Dybczynski and Krolikowska, 2011MNRAS.416...51D 2011MNRAS.416...51D
P3 = Krolikowska, Dybczynski and Sitarski, 2012A&A...544A.119K 2012A&A...544A.119K
P4 = Krolikowska and Dybczynski, 2013MNRAS.435..440K 2013MNRAS.435..440K
P5 = Krolikowska, 2014, Cat. J/A+A/567/A126
P6 = Krolikowska et al., 2014, Cat. J/A+A/571/A63
P7 = Krolikowska & Dybczynski, this paper (2017MNRAS.472.4634K 2017MNRAS.472.4634K)
Note (G3): in tables E3 and G3 the inverse of the semimajor axis, perihelion and
aphelion distances and the time intervals are all presented as two or
three numbers: the mean value and its standard deviation when the
swarm parameters follow the Gaussian distribution or three deciles
(10), (50 i.e.median) and (90).
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Acknowledgements:
Piotr A. Dybczynski, dybol(at)amu.edu.pl
Malgorzata Krolikowska, mkr(at)cbk.waw.pl
(End) Patricia Vannier [CDS] 12-Oct-2017