Searching for substellar companions of young isolated neutron stars

Posselt, Bettina; Neuhäuser, R.; Haberl, F.

doi:10.1051/0004-6361/200810156

Cited by 19 publications

(41 citation statements)

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“…For RX J2143.0+0654 (RBS 1774), the timing analysis by Kaplan & van Kerkwijk (2009b) gives P = 9.428 s anḋ P = 4.1(18) × 10 −14 s s −1 . The upper limit to the distance was given as 300 pc by Posselt, Neuhäuser & Haberl (2009) erg s −1 cm −2 by Kaplan et al (2003), which corresponds to a bolometric luminosity of ∼ 1.6 × 10 32 erg s −1 . In the present work, we have investigated the longterm evolution of these six XDINs (Table 1).…”

Section: Resultsmentioning

confidence: 99%

Long-term evolution of dim isolated neutron stars

Ertan¹,

Çalışkan²,

Benli³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The dim isolated neutron stars (XDINs) have periods in the same range as the anomalous X-ray pulsars (AXPs) and the soft gamma-ray repeaters (SGRs). We apply the fallback disk model, which explains the period clustering and other properties of AXP/SGRs, to the six XDINs with measured periods and period derivatives. Present properties of XDINs are obtained in evolutionary scenarios with surface dipole magnetic fields B 0 ∼ 10 12 G. The XDINs have gone through an accretion epoch with rapid spin-down earlier, and have emerged in their current state, with the X-ray luminosity provided by neutron star cooling and no longer by accretion. Our results indicate that the known XDINs are not likely to be active radio pulsars, as the low B 0 , together with their long periods place these sources clearly below the "death valley".

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Section: Resultsmentioning

confidence: 99%

Long-term evolution of dim isolated neutron stars

Ertan¹,

Çalışkan²,

Benli³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…If this is the case and RX J0720.4−3125 is precessing, then the precession needs to be powered by some mechanism. Precession caused by an unseen sub-stellar companion can probably be excluded on the basis of the current upper limit on its mass obtained by Posselt et al (2008) from a search for orbiting objects around RX J0720.4−3125 (see also the discussion on PSR B1828-11 by Liu et al 2006).…”

Section: Discussionmentioning

confidence: 99%

Spectral and temporal variations of the isolated neutron star RX J0720.4-3125: new XMM-Newton observations

Hohle

Haberl

Vink

et al. 2009

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Context. In the past, the isolated, radio-quiet neutron star RX J0720.4−3125 showed variations in its spectral parameters (apparent radius, temperature of the emitting area and equivalent width of the absorption feature) seen in the X-ray spectra, not only during the spin period of 8.39 s, but also over time scales of years. New X-ray observations of RX J0720.4−3125 with XMM-Newton extend the coverage to about 7.5 years with the latest pointing performed in November 2007. Out of a total of fourteen available EPIC-pn datasets, eleven have been obtained with an identical instrumental setup (full frame read-out mode with a thin filter), and are best suited for a comparative investigation of the spectral and timing properties of this enigmatic X-ray pulsar. Aims. We analysed the new XMM-Newton observations together with archival data in order to follow the spectral and temporal evolution of RX J0720.4−3125. Methods. All XMM-Newton data were reduced with the standard XMM-SAS software package. A systematic and consistent data reduction of all these observations is warranted in order to reduce systematic errors as far as possible. Results. We investigate the phase residuals derived from data from different energy bands using different timing solutions for the spin period evolution and confirm the phase lag between hard and soft photons. The phase shift in the X-ray pulses between hard and soft photons varies with time and changes sign around MJD = 52 800 days, regardless of the chosen timing solution. The phase residuals show a marked dependence on the energy band, and possibly follow a cyclic pattern with a period of ∼9-12 yrs. We find that an abs(sine) dependence provides a better fit to the residuals with respect to a simple sine wave, although in both cases the reduced χ 2 is not completely satisfactory. We compared the model fit to phase residuals derived from EPIC-MOS and Chandra (HRC and ACIS) data restricted to the hard energy band (400-1000 eV) to take into account the different energy responses of these instruments. Conclusions. The new data are not in contradiction with RX J0720.4−3125 being a precessing neutron star but do not provide overwhelming evidence for this picture either.

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“…The relevant information about these two pulsars is provided in Table I. Recall, the pulsar closest to the galactic center could be only ∼ 1 pc away from Sgr A * [36]; and the ones closest to the Earth are ∼ O(100) pc far (e.g., PSR J0108-1431 is at a distance ∼ 130 pc to the Earth [37]). The two benchmark pulsars thus represent a broad class of pulsars known to us.…”

Section: Pulsar-based Detectionmentioning

confidence: 99%

Detecting axionlike dark matter with linearly polarized pulsar light

2020

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Non-relativistic QCD axions or axion-like particles are among the most popular candidates for cold Dark Matter (DM) in the universe. We proposed to detect axion-like DM, using linearly polarized pulsar light as a probe. Because of birefringence effect potentially caused by an oscillating galactic axion DM background, when pulsar light travels across the galaxy, its linear polarization angle may vary with time. With a soliton+NFW galactic DM density profile, we show that this strategy can potentially probe an axion-photon coupling as small as ∼ 10 −13 GeV −1 for axion mass ma ∼ 10 −22 − 10 −20 eV, given the current measurement accuracy. An exclusion limit stronger than CAST (∼ 10 −10 GeV −1 ) and SN1987A (∼ 10 −11 GeV −1 ) could be extended up to ma ∼ 10 −18 eV and ∼ 10 −19 eV, respectively.

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Searching for substellar companions of young isolated neutron stars

Cited by 19 publications

References 50 publications

Long-term evolution of dim isolated neutron stars

Long-term evolution of dim isolated neutron stars

Spectral and temporal variations of the isolated neutron star RX J0720.4-3125: new XMM-Newton observations

Detecting axionlike dark matter with linearly polarized pulsar light

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