other query modes : |
Identifier query |
Coordinate query |
Criteria query |
Reference query |
Basic query |
Script submission |
TAP |
Output options |
Object types |
Help |
Query : 1999MNRAS.305..671B |
1999MNRAS.305..671B - Mon. Not. R. Astron. Soc., 305, 671-679 (1999/May-3)
The implications of radio-quiet neutron stars.
BRAZIER K.T.S. and JOHNSTON S.
Abstract (from CDS):
Quantitative upper limits exist for the radio fluxes of eight of the 10 objects, and reveal a population at least an order of magnitude less luminous at radio wavelengths than known radio pulsars of similar power or age. A simple explanation within the context of existing models is that these objects are pulsars in which the radio beams are directed away from Earth. They are still visible as X-ray sources because the thermal surface emission, which dominates the soft X-ray emission in most young to middle-aged radio pulsars, is radiated in all directions. In the cases where hard X-ray or γ-ray fluxes are seen, the beaming explanation implies different emission sites for the non-thermal high-energy radiation and the unseen radio beams. From the numbers of candidate neutron stars and radio pulsars younger than 20 000 yr and within 3.5 kpc, the radio beaming fraction of young pulsars is estimated to be roughly 50 per cent and certainly much less than 100 per cent. We find the local neutron star birth rate to be at least 13 Myr–1.kpc–2. This extrapolates to a Galactic rate of one neutron star born every ∼90 yr. We conclude that probably all neutron stars are born as radio pulsars, and that most young, nearby pulsars have already been discovered.
Abstract Copyright: 1999 RAS
Journal keyword(s): stars: neutron - X-rays: stars
CDS comments: 1E 1841-045 is 1E 1838-04.9
Simbad objects: 24
Number of rows : 24 |
N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2024 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | TYC 4018-3227-1 | * | 00 02 55.7100664872 | +62 46 17.662572696 | 12.49 | 11.67 | ~ | 40 | 1 | |||
2 | SNR G117.7+00.6 | SNR | 00 05 | +63.0 | ~ | 17 | 0 | |||||
3 | SNR G119.5+10.2 | SNR | 00 06.6 | +72 47 | ~ | 250 | 1 | |||||
4 | PSR J0007+7303 | Psr | 00 07 00.6000137 | +73 03 06.849976 | ~ | 171 | 1 | |||||
5 | SNR G130.7+03.1 | SNR | 02 05 37.0 | +64 49 42 | ~ | 620 | 4 | |||||
6 | NGC 1313 | AG? | 03 18 16.046 | -66 29 53.74 | 10.06 | 10.0 | 9.40 | 10.4 | ~ | 687 | 2 | |
7 | 2E 756 | ULX | 03 18 22.00 | -66 36 04.3 | 23.5 | 23.6 | O9.5 | 239 | 3 | |||
8 | M 1 | SNR | 05 34 30.9 | +22 00 53 | ~ | 6190 | 1 | |||||
9 | V* CM Tau | Psr | 05 34 31.9474694616 | +22 00 52.153698024 | ~ | 5256 | 0 | |||||
10 | NAME Geminga | Psr | 06 33 54.153 | +17 46 12.91 | ~ | 1221 | 0 | |||||
11 | NAME Pup A | BL? | 08 24 07 | -42 59.8 | ~ | 600 | 1 | |||||
12 | NAME Vela Pulsar | Psr | 08 35 20.65525 | -45 10 35.1545 | 15.10 | ~ | 2314 | 1 | ||||
13 | PSR B1046-58 | Psr | 10 48 13.0500 | -58 32 06.200 | ~ | 268 | 0 | |||||
14 | AJG 14 | BL? | 12 09 40 | -52 25.0 | ~ | 287 | 1 | |||||
15 | PSR J1210-5226 | Psr | 12 10 00.88 | -52 26 28.4 | ~ | 225 | 1 | |||||
16 | AJG 44 | Psr | 16 17 33.000 | -51 02 00.00 | ~ | 512 | 3 | |||||
17 | PSR B1706-44 | Psr | 17 09 42.7460 | -44 29 07.200 | 13.30 | ~ | 640 | 1 | ||||
18 | PSR B1737-30.2 | Psr | 17 40 33.82 | -30 15 43.5 | ~ | 214 | 0 | |||||
19 | RX J1838.4-0301 | XB* | 18 38 27.02 | -03 01 14.4 | ~ | 29 | 0 | |||||
20 | 4C -04.71 | Rad | 18 41 19.8 | -04 56 06 | ~ | 326 | 3 | |||||
21 | RX J1856.6-3754 | Psr | 18 56 35.11 | -37 54 30.5 | 25.7 | ~ | 437 | 0 | ||||
22 | RX J2020.3+4026 | X | 20 20 17.1 | +40 26 09 | ~ | 12 | 1 | |||||
23 | NAME gam Cyg SNR | BL? | 20 20 17.100 | +40 26 09.00 | ~ | 229 | 2 | |||||
24 | 2E 4673 | HXB | 23 01 08.14 | +58 52 44.5 | ~ | 633 | 1 |
To bookmark this query, right click on this link: simbad:objects in 1999MNRAS.305..671B and select 'bookmark this link' or equivalent in the popup menu