Chandra
 and
 XMM
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 Newton
 Observations of the Exceptional Pulsar B0628-28

Tepedelenlioǧlu, E.; Öğelman, H.

doi:10.1086/444360

Cited by 16 publications

(14 citation statements)

References 8 publications

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“…Although it also satisfies equation (1), it predicts a very high polar cap heating rate, typically L b $ 10 À1 10 À2 ð ÞĖ , and therefore a very small P 4 . The predicted high L b has been ruled out by the X-ray observations of many old pulsars (Zhang et al 2005;Tepedelenlioglu & Ö gelman 2005;Kargaltsev et al 2006; this paper), and the predicted low P 4 is also inconsistent with radio observations. On the other hand, as discussed in x 1, the steady state SCLF model does not predict the existence of the ''sparks,'' whose drifts around the polar cap region provide the most natural interpretation of the observed drifting-subpulse patterns.…”

Section: Conclusion and Discussionmentioning

confidence: 68%

“…As indicated in Table 1, it was detected in X-rays by Tepedelenlioglu & Ö gelman (2005) using Chandra and XMMNewton. This was an exceptional pulsar (called ''overluminous'' by Becker et al 2005) with an efficiency much larger than that of typical pulsars (Becker & Trümper 1997).…”

Section: Previous Workmentioning

confidence: 92%

“…References.-(1) Deshpande & Rankin 1999; (2) Paper I; (3) HR07; (4) RW07; (5) this paper; (6) Paper II; (7) Biggs (1990); (8) Gupta et al 2004;(9) Zhang et al 2005; (10) Kargaltsev et al 2006;(11) M07; (12) DL05; (13) Tepedelenlioglu & Ö gelman 2005. polar cap (again much smaller-by about 100 times-than the canonical one). As one can see in Figure 1, with the inferred values of P 4 and L b , the pulsar B1133+16 nicely clusters with its twin along the critical curve expressed by equation (1).…”

Section: Previous Workmentioning

confidence: 99%

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XMM‐NewtonObservations of Radio Pulsars B0834+06 and B0826−34 and Implications for the Pulsar Inner Accelerator

Gil

Haberl

Melikidze

et al. 2008

Astrophysical Journal

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We report the X-ray observations of two radio pulsars with drifting subpulses, B0834+06 and B0826À34, using XMM-Newton. PSR B0834+06 was detected with a total of 70 counts from the three EPIC instruments over 50 ks exposure time. Its spectrum is best described as that of a blackbody (BB), with temperature T s ¼ (2:0 þ2:0 À0:9 ) ; 10 6 K and bolometric luminosity L b ¼ (8:6 þ14:2 À4:4 ) ; 10 28 erg s À1 . As is typical in pulsars with BB thermal components in their X-ray spectra, the hot-spot surface area is much smaller than that of the canonical polar cap, implying a non-dipolar surface magnetic field much stronger than the dipolar component derived from the pulsar spin-down (in this case about 50 times smaller and stronger, respectively). The second pulsar, PSR B0826À34, was not detected over the 50 ks exposure time, giving an upper limit for the bolometric luminosity L b 1:4 ; 10 29 erg s À1 . We use these data, as well as the radio emission data concerned with drifting subpulses, to test the partially screened gap ( PSG) model of the inner accelerator in pulsars. This model predicts a simple and very intuitive relationship between the polar cap thermal X-ray luminosity (L b ) and the ''carousel'' period (P 4 ) for drifting subpulses detected in the radio band. The PSG model has been previously successfully tested with four radio pulsars whose L b and P 4 were both measured: PSR B0943+10, PSR B1133+16, PSR B0656+14, and PSR B0628À28. The XMM-Newton X-ray data of PSR B0834+16 reported here are also in agreement with the model prediction, and the upper limit derived from the PSR B0826À34 observation does not contradict it. We also include two other pulsars, PSR B1929+10 and B1055À52, whose L b and/or P 4 data became available just recently. These pulsars also follow the prediction of the PSG model. The clear prediction of the PSG model is now supported by all pulsars whose L b and P 4 are measured and/or estimated.

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Section: Conclusion and Discussionmentioning

confidence: 68%

Section: Previous Workmentioning

confidence: 92%

Section: Previous Workmentioning

confidence: 99%

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XMM‐NewtonObservations of Radio Pulsars B0834+06 and B0826−34 and Implications for the Pulsar Inner Accelerator

Gil

Haberl

Melikidze

et al. 2008

Astrophysical Journal

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“…One could argue that the PL fits to the spectra of other old pulsars (e.g., B0950+08, B2224+65, B0823+26, B0628À28,B1133+16, B0943+10; Zavlin & Pavlov 2004;Becker et al 2004;Tepedelenl5oǧlu & Ö gelman 2005;Kargaltsev et al 2006a;Zhang et al 2005) also show rather steep slopes, À % 2Y3, suggesting that pulsar spectra might soften with increasing age or decreasing spin-down power (Kargaltsev et al 2006a). However, a plausible alternative interpretation of the softer spectra of old pulsars is that they are, in fact, composed of a (soft) thermal component and a PL component with a more gradual slope, 8 similar to those found in young pulsars (Zavlin & Pavlov 2004).…”

Section: Spectral Properties Of Psr B1929+10mentioning

confidence: 99%

ChandraObservations of the Pulsar B1929+10 and Its Environment

Misanovic

Pavlov

Garmire

2008

Astrophysical Journal

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We report on two Chandra observations of the 3 Myr old pulsar B1929+10, which reveal a faint compact ($9 00 ; 5 00 ) nebula elongated in the direction perpendicular to the pulsar's proper motion, two patchy wings, and a possible short ($3 00 ) jet emerging from the pulsar. In addition, we detect a tail extending up to at least 4 0 in the direction opposite to the pulsar's proper motion, aligned with the $15 0 long tail detected in ROSAT and XMM-Newton observations. The overall morphology of the nebula suggests that the shocked pulsar wind is confined by the ram pressure due to the pulsar's supersonic speed. The shape of the compact nebula in the immediate vicinity of the pulsar seems to be consistent with the current MHD models. However, since these models do not account yet for the change of the flow velocity at larger distances from the pulsar, they are not able to constrain the extent of the long pulsar tail. The luminosity of the whole nebula as seen by Chandra is L PWN $ 10 30 ergs s À1 in the 0.3Y8 keV band, for the distance of 361 pc. Using the Chandra and XMM-Newton data, we found that the pulsar spectrum is composed of nonthermal (magnetospheric) and thermal components. The nonthermal component can be described by a power-law model with photon index À % 1:7 and luminosity L nonth PSR % 1:7 ; 10 30 ergs s À1 in the 0.3Y10 keV band. The blackbody fit for the thermal component, which presumably emerges from hot polar caps, gives the temperature kT % 0:3 keV and projected emitting area A ? $ 3 ; 10 3 m 2 , corresponding to the bolometric luminosity L bol $ (1Y2) ; 10 30 ergs s À1 .

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“…A growing sample of pulsars in this age group have been observed by X‐ray observatories ( Chandra and XMM–Newton ; e.g. Becker et al 2004, 2005; Zavlin & Pavlov 2004; De Luca et al 2005; Zhang, Sanwal & Pavlov 2005; Tepedelenliolu & Ögelman 2005; Kargaltsev et al 2006). These observations indicate that the emission of these pulsars likely has multiple emission components, including a non‐thermal magnetospheric component and sometimes a hotspot thermal emission component.…”

Section: X‐rays As Possible Differentiatormentioning

confidence: 99%

On the origins of part-time radio pulsars

Zhang

Gil

Dyks

2007

Monthly Notices of the Royal Astronomical Society

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Growing evidence suggests that some radio pulsars only act sporadically. These "part-time'' pulsars include long-term nulls, quasi-periodic radio flares in PSR B1931+24, as well as the so-called Rotating RAdio Transients (RRATs). Based on the assumption that these objects are isolated neutron stars similar to conventional radio pulsars, we discuss two possible interpretations to the phenomenon. The first interpretation suggests that these objects are pulsars slightly below the radio emission "death line'', which become active occasionally only when the conditions for pair production and coherent emission are satisfied. The second interpretation invokes a radio emission direction reversal in conventional pulsars, as has been introduced to interpret the peculiar mode changing phenomenon in PSR B1822-09. In this picture, our line of sight misses the main radio emission beam of the pulsar but happens to sweep the emission beam when the radio emission direction is reversed. These part-time pulsars are therefore the other half of "nulling'' pulsars. We suggest that X-ray observations may provide clues to differentiate between these two possibilities.Comment: Expanded version to include more general discussion of part-time pulsars. Accepted to MNRA

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Chandra and XMM - Newton Observations of the Exceptional Pulsar B0628-28

Cited by 16 publications

References 8 publications

XMM‐NewtonObservations of Radio Pulsars B0834+06 and B0826−34 and Implications for the Pulsar Inner Accelerator

XMM‐NewtonObservations of Radio Pulsars B0834+06 and B0826−34 and Implications for the Pulsar Inner Accelerator

ChandraObservations of the Pulsar B1929+10 and Its Environment

On the origins of part-time radio pulsars

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