Table 2

Comet type and classification with observed main species and hydrocarbons at comets.

Type Comet Classification H2O CO CO2 CH4 C2H2 C2H6

HTC 1P/Halley T[A,B] 100 3.5a,[1]; 11b,[1]; 3-4[2]; 3.5[3]; <1[4]; 0.6[5] 0.3[1,5] 0.4[1,5]
H(CH, C 13b,[5] 2.5[5]
LPC C/1995 O1 (Hale-Bopp) T[B]; D[D] 100 12[6]; 23[6,7] 6[8] 1.5[9] 0.1[9]; 0.3[10]; 0.6[10]
H(CH, C3)[C] 0.2[11]
LPC C/1996 B2 (Hyakutake) T[B,C] 100 14[12,13]; 0.8[9,16] 0.2[17]; 0.5[18] 0.6[16]
19-30[12,14,15]
LPC C/2001 A2 (LINEAR) T[C] 100 3.9[19]; <3.7[39] 1.2[40]; 0.5[19] 1.7[19]
LPC C/2012 F6 (Lemmon) 100 4.03[20] 0.67[20] <0.05[20]
LPC C/2013 R1 (Lovejoy) 100 7.2[21]
JFC 103P/Hartley 2 100 0.15–0.45[22] 7[23]; 8[24]; 0.08[26]; 0.75[26]
<1[23] 20[25] 0.13–0.16[27] 0.63–0.93[27]
0.08–0.13[41] 0.71–0.95[41]
JFC 73P/SW3/B D[28] 100 <1.9[28] <0.06–0.026[28] 0.136–0.193[28];
<0.3[29]
JFC 73P/SW3/C D[28] 100 <2.6[28]; 0.5[30] <0.25-0.39[29] <0.033–0.049[28]; 0.23[29] 0.065-0.119[28];
0.15[29]
JFC 2P/Encke T[A,B]; H(CH)[C]; 100 <1.77[31] 0.34[31] <0.08[31] 0.32[31]
L(NH)[C]
JFC 9P/Tempel 1 before impact T[A,C]; L(C2)[B]; D[D] 100 <10[32] 0.19[33]; 0.278[42]
JFC 9P/Tempel 1 after impact 100 <32[32]; 4.3[33] 0.54[33] 0.13[33] 0.35[33]
0.199–0.397[42]
JFC 6P/d’Arrest T[A,B,C] 100 <0.052[34] 0.26[34]
JFC 17P/Holmes 100 0.344[35] 1.78[35]
JFC 21P/Giacobini-Zinner D[A,C] 100 10[36]; 0.28–0.42[37] 0.2[36]; 0.05–0.08[37]
L(C2, NH2)[B] 2.1–3.2[37]
JFC 67P T[C]; D[A]; L(C2)[B] 100 <22[38] 7[38]
JFC 67P summer hemisphere D[43] 100[43] 2.7[43] 2.5[43] 0.13[43] 0.045[43] 0.32[43]
JFC 67P winter hemisphere T[43] 100[43] 20[43] 80[43] 0.56[43] 0.55[43] 3.3[43]

Notes. This table is based on Table 1 in Bockelée-Morvan et al. (2004) and Table 4 in Mumma & Charnley (2011). The classification is based on Table 8 in Cochran et al. (2012), see notes and the references below. HTC, LPC, and JFC stand for Halley-type comet, long-period comet and Jupiter-family comet. References for the abundances: [1] Eberhardt (1999); [2] Combes et al. (1988); [3] Krankowsky et al. (1986); [4] Altwegg et al. (1994); [5] Rubin et al. (2011); [6] DiSanti et al. (2001); [7] Bockelée-Morvan et al. (2000); [8] Crovisier et al. (1997); [9] Gibb et al. (2003); [10] Dello Russo et al. (2001); [11] Despois et al. (2005); [12] DiSanti et al. (2003); [13] McPhate et al. (1996); [14] Biver et al. (1999); [15] Lis et al. (1997a); [16] Mumma et al. (1996); [17] Mumma et al. (2003); [18] Brooke et al. (1996); [19] Magee-Sauer et al. (2008) (9.5 July 2001); [20] Paganini et al. (2014); [21] Biver et al. (2014); [22] Weaver et al. (2011); [23] Weaver et al. (1994); [24] Colangeli et al. (1999); [25] A’Hearn et al. (2011); [26] Mumma et al. (2011), (22 October 2010); [27] Dello Russo et al. (2011); [28] Dello Russo et al. (2007); [29] Villanueva et al. (2006) ; [30] DiSanti et al. (2007a); [31] Radeva et al. (2013); [32] Biver et al. (2007); [33] Mumma et al. (2005); [34] Dello Russo et al. (2009) (11 August 2008); [35] Dello Russo et al. (2008) (27.6 October 2008, rh = 2.45 AU); [36] Mumma et al. (2000) (values for Trot = 35 K); [37] Weaver et al. (1999); [38] Ootsubo et al. (2012); [39] Biver et al. (2006) (values at 1.1 AU); [40] Gibb et al. (2007) (global mixing ratio, 9.5 July 2001); [41] Kawakita et al. (2013); [42] DiSanti et al. (2007b); [43] this work; abundance comments: notes for the classification : T = typical; D = depleted ; L(X) = low X; H(X) = high X; references for the classification: [A] A’Hearn et al. (1995); [B] Fink (2009); [C] Cochran et al. (2012); [D] Langland-Shula & Smith (2011).

(a)

CO from the nucleus,

(b)

CO from extended source;

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