2011MNRAS.417..617T


Query : 2011MNRAS.417..617T

2011MNRAS.417..617T - Mon. Not. R. Astron. Soc., 417, 617-626 (2011/October-2)

The origin of RX J1856.5-3754 and RX J0720.4-3125 – updated using new parallax measurements.

TETZLAFF N., EISENBEISS T., NEUHAUSER R. and HOHLE M.M.

Abstract (from CDS):

RX J1856.5-3754 and RX J0720.4-3125 are the only young isolated radio-quiet neutron stars (NSs) for which trigonometric parallaxes were measured. Due to detection of their thermal emission in X-rays, they are important to study NS cooling and to probe theoretical cooling models. Hence, a precise determination of their age is essential.

Recently, new parallax measurements of RX J1856.5-3754 and RX J0720.4-3125 were obtained. Considering that NSs may originate from binary systems that got disrupted due to an asymmetric supernova, we attempt to identify runaway stars which may have been former companions to the NS progenitors. Such an identification would strongly support a particular birth scenario with time and place.

We trace back each NS, runaway star and the centres of possible birth associations (assuming that most NSs are ejected directly from their parent association) to find close encounters. The kinematic age is then given by the time since the encounter. We use Monte Carlo simulations to account for observational uncertainties and evaluate the outcome statistically.

Using the most recent parallax measurement of 8.16±0.80 mas for RX J1856.5-3754 by (Walter et al.), we find that it originated in the Upper Scorpius association 0.46±0.05 Myr ago. This kinematic age is slightly larger than the value we reported earlier (0.3 Myr) using the old parallax value of 5.6±0.6 mas by (Kaplan). Our result is strongly supported by its current radial velocity which we predict to be 6+19_- 20_ km/s. This implies an inclination angle to the line of sight of 88°± 6° consistent with estimates by (van Kerkwijk & Kulkarni) from the bow shock. No suitable runaway star was found to be a potential former companion of RX J1856.5-3754.

Making use of a recent parallax measurement for RX J0720.4-3125 of 3.6±1.6 mas by (Eisenbeiss), we find that this NS was possibly born in Trumpler 10 0.85±0.15 Myr ago. This kinematic age is somewhat larger than the one obtained using the old parallax value of 2.77±1.29 mas by (Kaplan et al.) (0.5 Myr). We suggest the B0 runaway supergiant HIP 43158 as a candidate for a former companion of the progenitor star. Then, the current distance of RX J0720.4-3125 to the Sun should be 286+27_- 23_pc, in agreement with recent measurements. We then expect the radial velocity of RX J0720.4-3125 to be -76+34_- 17_ km/s.


Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): stars: kinematics and dynamics - pulsars: individual: RX J0720.4-3125 - pulsars: individual: RX J1856.5-3754

Simbad objects: 60

goto Full paper

goto View the references in ADS

Number of rows : 60
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME THA As* 00 00 -62.0           ~ 424 0
2 HIP 17158 PM* 03 40 29.5129917672 +05 07 47.634942648   10.11 9.58     G0 15 0
3 HD 25457 TT* 04 02 36.7442719512 -00 16 08.119921152   5.88 5.38     F7V 254 0
4 HD 25953 PM* 04 06 41.5332077256 +01 41 02.078668860   8.32 7.82     F6V 57 1
5 NAME Columba Association As* 06 04 19.4 -22 20 40           ~ 254 0
6 NAME AB Dor Moving Group MGr 06 38 53.4 -42 50 04           ~ 433 0
7 RX J0720.4-3125 N* 07 20 24.961 -31 25 50.21   26.1   27.0   ~ 292 0
8 Cl Collinder 140 OpC 07 23 32 -31 58.0           ~ 119 0
9 HD 59100 PM* 07 26 57.6339225128 -34 18 55.888953479   8.82 8.19     G1.5V 48 0
10 * h02 Pup SB* 08 14 02.9293688256 -40 20 52.321700292 6.70 5.61 4.44 3.60 2.96 K1II/III 42 0
11 V* IX Vel CV* 08 15 18.9688659456 -49 13 20.671780368 8.64 10.04 10.10 9.84 9.347 sdOBe 230 0
12 PSR J0821-4300 Psr 08 21 58.2 -43 00 22           ~ 120 2
13 HD 75222 s*b 08 47 25.1378783304 -36 45 02.670440616 7.24 7.80 7.42 8.22   O9.7Iab 86 0
14 Cl Trumpler 10 OpC 08 47 46 -42 34.0           ~ 158 0
15 * y Vel Pe* 09 38 01.4514238848 -43 11 27.384240840 7.18 6.50 5.50     G8IIIBa1.5 122 0
16 NAME TW Hya Association As* 11 01.9 -34 42           ~ 897 0
17 HD 102077 BY* 11 44 38.4210169656 -49 25 02.404105608   10.04 8.917   7.831 K1V 93 0
18 * gam Crv PM* 12 15 48.37081 -17 32 30.9496 2.12 2.47 2.58 2.62 2.71 B8III 232 0
19 HD 113564 * 13 04 38.5291888344 -00 43 41.914041744   8.58 7.19     K0/1III 15 0
20 HD 113778 V* 13 06 35.0821484352 -41 35 18.397334724   6.641 5.588     K0II/III 24 0
21 HD 120559 PM* 13 51 40.3987847839 -57 26 08.350982731 8.679 8.647 7.982 7.605 7.217 G7VFe-1.4CH-1 149 0
22 HD 121967 PM* 13 58 40.3421063616 +09 18 37.643704740   9.04 8.81     A2 13 0
23 HD 122948 PM* 14 04 43.2065903088 +04 46 45.799527540       8.1   G5 22 0
24 HD 126231 * 14 24 34.7291365464 -11 05 49.137787356   9.21 8.99     A3III 9 0
25 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 691 0
26 PSR B1508+55 Psr 15 09 25.674 +55 31 32.90           ~ 281 1
27 HD 134339 ** 15 10 00.22536 -22 43 14.8307   8.55 8.10     F5V 11 1
28 HD 135485 SB* 15 15 45.2566709328 -14 41 34.523913444 7.57 8.05 8.13     B3V 111 0
29 * 4 Ser PM* 15 15 49.0775968992 +00 22 19.695424008   5.800 5.623     A5V 51 0
30 HD 135449 Pe* 15 16 10.3868491680 -32 53 33.070359120   9.78 9.46     F/Gw 48 0
31 BD-19 4128B PM* 15 31 42.6243379536 -20 09 51.804224280   9.40 8.89     F0 25 0
32 HD 138779 PM* 15 35 13.6565847264 -28 28 27.673779108   8.72 8.13     G2V 33 0
33 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 505 0
34 V* HR Lib dS* 15 56 33.3736378344 -14 49 45.972944112   6.345 6.117     A2Ib/II 112 0
35 * ksi02 Lup * 15 56 54.1128088176 -33 57 51.338030580   5.61 5.55     B9V 48 0
36 HD 143899 SB* 16 03 43.8067112448 -19 34 30.730124064   9.35 8.30     G8IIBa1 35 0
37 NAME Upper Sco Association As* 16 12 -23.4           ~ 1222 1
38 HD 145518 PM* 16 12 02.4536629920 -18 13 57.439412148   8.02 7.41     G0.5V 42 0
39 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1247 1
40 * tau Sco * 16 35 52.9528530 -28 12 57.661515 1.55 2.56 2.81 2.93 3.18 B0.2V 892 0
41 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1792 2
42 Ass Sco OB 4 As* 17 12.6 -33 22           ~ 43 0
43 Cl VDBH 217 OpC 17 16 17 -40 48.9           ~ 26 0
44 Ross 868 Er* 17 19 54.2077697528 +26 30 03.068999297   12.98 11.336 11.060 8.420 M3.5V 155 0
45 Cl Pismis 24 OpC 17 24 43.0 -34 12 23           ~ 117 0
46 NGC 6383 OpC 17 34 42 -32 34.4           ~ 150 0
47 Cl Trumpler 27 OpC 17 36 20 -33 31.0   8.24 6.7     ~ 96 1
48 NGC 6396 OpC 17 37 36 -35 00.8   9.41 8.5     ~ 41 0
49 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13202 0
50 Ass Sgr OB 5 As* 17 50 -29.6           ~ 21 0
51 RX J1856.6-3754 Psr 18 56 35.11 -37 54 30.5     25.7     ~ 414 0
52 PSR B2223+65 Psr 22 25 52.36 +65 35 33.8           ~ 310 0
53 NAME R CrA Association As* ~ ~           ~ 20 0
54 NAME Vela Field reg ~ ~           ~ 164 0
55 NAME Hercules-Lyra Moving Group MGr ~ ~           ~ 61 0
56 NAME Argus Association As* ~ ~           ~ 206 0
57 NAME Local Bubble ISM ~ ~           ~ 805 0
58 NAME Magnificent Seven ? ~ ~           ~ 65 1
59 NAME Octans Association As* ~ ~           ~ 81 0
60 NAME Carina Association As* ~ ~           ~ 138 1

To bookmark this query, right click on this link: simbad:objects in 2011MNRAS.417..617T and select 'bookmark this link' or equivalent in the popup menu


2022.10.05-19:28:09

© Université de Strasbourg/CNRS

    • Contact