Engineering topics

Finley, John P.

Publications and source records attributed to Finley, John P..

8 records

NASA NTRS1997

Vela-like Pulsars: A Bridge Between Young and Old

This grant was in support of a guest observation using the ASCA satellite of the young, spin-powered pulsar PSR B1706-44. The pulsar is interesting for several reasons: 1) it is young and shares many similar characteristics with the Vela pulsar, 2) it is one of a few pulsars which has been detected by the EGRET detector aboard the CGRO satellite, and 3) it is one of the confirmed sources of TeV gamma-rays discovered with ground based telescopes. The goals of the observation were to search for pulsations in the X-ray domain and to study the near stellar environment to determine if the pulsar is embedded within a compact nebula as in the case of the Vela pulsar.

Finley, John P.↗

NASA NTRS1995

ROSAT observations of the unusual supernova remnant CTB 80 containing the pulsar PSR 1951 + 32

The unusal supernova remnant CTB, 80 containing the 39.5 ms pulsar PSR 1951 + 32, has been observed with the Position Sensitive Proportional Counter (PSPC) and the High Resolution Imager (HRI) aboard ROSAT. The HRI image, centered on the pulsar, is composed of a bright compact core of approximately 1 arcminute radius containing the pulsar and a compact nebula, as well as a diffuse nebula extending approximately 5 arcminutes eastward of the pulsar. The PSPC allowed us to model the spectra of the point source, the compact nebula and the 5 arcminute diffuse nebula. For a power-law spectrum with photon index Gamma approximately 2 and an interstellar column density of N(sub H) approximately 3 x 10(exp 21)/cm(exp 21) the derived luminosities are approximately 2.3 x 10(exp 33) d(sub 2.5)(exp 2) ergs/s from the pointlike source, approximately 3.9 x 10(exp 33) d(sup 2.5)(exp 2) ergs/s from the compact nebula, and approximately 1.8 x 10(exp 33) d(sub 2.5)(exp 2) ergs/s from the 5 arcminutes diffuse nebula. In addition, the 2 deg diameter circular field of view of the PSPC reveals a hard emission feature southeast of the pulsar with a conical geometry extending out to the edge of the detector. The spectrum from this region is well described by a two-temperature Raymond-Smith thermal plasma with an average temperature of approximately 10(exp 7) K and a luminosity of approximately 10(exp 34)d(sub 2.5)(exp 2) ergs/s. Pulsations from the 39.5 ms puslar, PSR 1951 + 32, are detected at the 99% confidence level. The implied pulsed fration is approximately 35% with a complicated energy-dependent behavior. The compact core and the extended diffuse nebula can be explained as synchrotron radiation from the relativistic pulsar wind confined by the ram pressure of the surrounding inhomgeneous medium. The conelike feature detected southeast of PSR 1951 + 32 is consistent with emission from an optically thin SNR in the radiative cooling phase of its evolution.

Safi-Harb, Samar↗

NASA NTRS1994

The PSR 1800-21/G8.7-0.1 association: A view from ROSAT

We present the first imaging X-ray observation of the W30 complex which contains the Galactic SNR G8.7-0.1 and the young radio pulsar PSR 1800-21 as well as a number of discrete ultracompact H II regions. The pulsar PSR 1800-21 is detected as a count rate of 1.5 +/- 0.5/ks and diffuse emission from the northern extent of G8.7-0.1 observed. The data support an association of G8.7-0.1 and PSR 1800-21, and the peculiar morphology can be explained if the supernova which gave birth to PSR 1800-21 occurred within, or very near, a molecular cloud. The suggested scenario removes the requirement of a large transverse velocity for the pulsar, one of the greatest dificulties with the association.

Finley, John P.↗

NASA NTRS1994

ROSAT/optical observations of 2S 0114 + 65: A study of the 2.8 hour periodic outbursts

Observations of the massive X-ray binary 2S 0114 + 65 acquired in 1992 July with the ROSAT Position Sensitive Proportional Counter (PSPC) in the 0.1-2.4 keV X-ray band and in 1992 September with the 0.9 m telescope at Kitt Peak National Observatory (KPNO) in the optical V band are reported. The X-ray data confirm the presence of persistent 2.78 hr outbursts as previously deduced from archival data. The X-ray source displays apparent orbital effects consistent with noncircularity. Variable intrinsic absorption and intrinsic spectral variations are excluded as the cause of the X-ray modulation. The optical V-band photometic data do not reveal any periodic modulation. The possibilty that the 2.78 hr period is the rotation of the neutron star component is entertained.

Finley, John P.↗

NASA NTRS1993

ROSAT observations of pulsed soft X-ray emission from PSR 1055-52

Utilizing the position-sensitive proportional counter and the high-resolution imager aboard the orbiting X-ray observatory ROSAT, we have detected pulsations at the radio period from the pulsar PSR 1055-52. The pulse shapes are energy-dependent and show a transition at about 0.5 keV where the phase angle of the pulse peak changes by about -120 deg and the pulsed fraction increases from 11 percent to 63 percent toward larger energies. Simple spectral models are found to be unsatisfactory, while multicomponent models, such as a soft blackbody and hard power-law tail, yield better fits to the pulse-height data. The hard power-law tail is consistent with the extension of the recently reported EGRET results and may indicate a common emission mechanism for the X-ray through GeV gamma-ray regime. The soft blackbody component with T(infinity) = (7.5 +/- 0.6) x 10 exp 5 K, if interpreted as the initial cooling of a neutron star, is consistent with standard cooling models and does not require the presence of exotic components.

Oegelman, Hakki↗

NASA NTRS1993

ROSAT observations of the LMC pulsar PSR 0540-69

Observations of the LMC pulsar PSR 0540-69 acquired during June-July 1990 and February 1991 with the Position Sensitive Proportional Counter on board ROSAT are reported, as are the results of timing and spectral analyses. The timing data are consistent with contemporaneous optical ephemerides, suggesting that the optical and X-ray pulses are in phase. The timing properties are used to ascertain the spectral characteristics of the pulsar and nebula separately. The spectral index of the pulsed component is determined using solely X-ray data. While many of the characteristics of the LMC pulsar are found to be similar to those of the Crab, the differences have yet to be explained.

Finley, John P.↗

NASA NTRS1992

Rotational parameters of PSR 0540 - 69 as measured at optical wavelengths

The rotation frequency of the 50 ms pulsar PSR 0540 - 69 utilizing data collected at the ESO 3.6 m telescope at La Silla is measured. The observations were acquired in the interval 1989 January-1991 April. The average pulse shape displays a broad enhancement with a superposed double-peaked structure. It was possible to phase-relate the data between 1990 March and 1991 April indicating the pulsar did not display any large spin discontinuities during that time span. Three solutions, incorporating a pulse number ambiguity of +/- 1, are presented. The preferred solution yields a braking index of 2.04 +/- 0.02, comparable with GINGA measurements in 1987. Discrepancies between these results and extrapolation of the GINGA results are discussed.

Gouiffes, Christian↗

NASA NTRS1992

Rosat observations of PSR 0656 + 14 - A pulsating and cooling neutron star

Observations of the X-ray-emitting radio pulsar PSR 0656 + 14 with the Position Sensitive Proportional Counter on board Rosat on March 25, 1991 are reported. Pulsations at the radio period, about 0.385 s, were detected at a pulsed fraction of 14 +/-2 percent. A blackbody description yields a surface temperature of about (9.0 +/-0.4) x 10 exp 5 K, an equivalent column density of about (1.0 +/-0.2) x 10 exp 20/sq cm, and a stellar radius of 10 km under the assumption of a 500 pc source distance. A positive correlation is found to exist between the phase of the pulsed emission and the X-ray hardness, suggesting that the pulsations have their seat in a 'hot spot' on the neutron star surface. Implications of the models with regard to the cooling curve of neutron stars are discussed.

Finley, John P.↗