The birthrate of magnetars

Gill, Ramandeep

doi:10.1111/j.1365-2966.2007.12254.x

Cited by 38 publications

(43 citation statements)

References 37 publications

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“…(5) in OLNIII) this gives a birthrate of (1 per 1000 years) to (1 per 100 years). Within uncertainties, the birth rate of transient AXPs derived above is consistent with the expected birthrate of AXPs (∼1/300 yrs; Gill & Heyl 2007;). As we argued in the previous section, in our model transient AXPs evolve into typical AXPs thus sharing the same birthrate.…”

Section: Birthratesupporting

confidence: 61%

Quark-nova remnants

Ouyed¹,

Leahy²,

Niebergal³

2010

A&A

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XTE J1810−197 and 1E 1547.0−5408 are two transient anomalous X-rays pulsars (AXPs) exhibiting radio emission with unusual properties. In addition, their spin down rates during outburst show opposite trends, which so far has no explanation. Here, we extend our quark-nova model for AXPs to include transient AXPs, in which the outbursts are caused by transient accretion events from a Keplerian (iron-rich) degenerate ring. For a ring with inner and outer radii of 23.5 km and 26.5 km, respectively, our model gives a good fit to the observed X-ray outburst from XTE J1810−197 and the behavior of temperature, luminosity, and area of the two X-ray blackbodies with time. The two blackbodies in our model are related to a heat front (i.e. Bohm diffusion front) propagating along the ring's surface and an accretion hot spot on the quark star surface. Radio pulsations in our model are caused by dissipation at the light cylinder of magnetic bubbles, produced near the ring during the X-ray outburst. The delay between X-ray peak emission and radio emission in our model is related to the propagation time of these bubbles to the light cylinder and scale with the period as t prop. ∝ P 7 2 − α 2 /Ṗ 1/2 where α defines the radial dependence of matter density in the magnetosphere (∝r −α ); for an equatorial wind, α = 1, we predict a ∼1 year and ∼1 month delay for XTE J1810−197 and 1E 1547.0−5408, respectively. The observed flat spectrum, erratic pulse profile, and the pulse duration are all explained in our model as a result of X-point reconnection events induced by the dissipation of the bubbles at the light cylinder. The spin down rate of the central quark star can either increase or decrease depending on how the radial drift velocity of the magnetic islands changes with distance from the central star. We suggest an evolutionary connection between transient AXPs and typical AXPs in our model.

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Section: Birthratesupporting

confidence: 61%

Quark-nova remnants

Ouyed¹,

Leahy²,

Niebergal³

2010

A&A

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“…In each part of our study (log N –log S for the M7, log N –log L for magnetars, for PSRs), we model ‘just NSs’ using the same initial magnetic field distribution (which in our model is the main parameter), without specifying unique particular features for a given subpopulation, as it is usually done (see e.g. Popov, Turolla & Possenti 2006; Gill & Heyl 2007; Keane & Kramer 2008).…”

Section: Discussion and Final Remarksmentioning

confidence: 99%

Population synthesis studies of isolated neutron stars with magnetic field decay

Попов¹,

Pons

Miralles

et al. 2010

Monthly Notices of the Royal Astronomical Society

142

192

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We perform population synthesis studies of different types of neutron stars (NSs) (thermally emitting isolated NSs, normal radio pulsars, magnetars) taking into account the magnetic field decay and using results from the most recent advances in NS cooling theory. For the first time, we confront our results with observations using simultaneously the log N–log S distribution for nearby isolated NSs, the log N–log L distribution for magnetars, and the distribution of radio pulsars in the diagram. For this purpose, we fix a baseline NS model (all microphysics input), and other relevant parameters to standard values (velocity distribution, mass spectrum, birth rates, etc.), allowing us to vary the initial magnetic field strength. We find that our theoretical model is consistent with all sets of data if the initial magnetic field distribution function follows a lognormal law with 〈log (B0/G)〉∼ 13.25 and . The typical scenario includes about 10 per cent of NSs born as magnetars, significant magnetic field decay during the first million years of a NS life (only about a factor of 2 for low‐field NSs but more than an order of magnitude for magnetars), and a mass distribution function dominated by low‐mass objects. This model explains satisfactorily all known populations. Evolutionary links between different subclasses may exist, although robust conclusions are not yet possible.

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“…The rate of magnetars is widely uncertain, but such values are advocated by some authors [37]. One may note furthermore that these rates includes mostly neutron stars that are are born with relatively low rotation periods (Ω i,min ∼ 300 s −1 , for µ 33 ).…”

Section: Figmentioning

confidence: 99%

Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures

Kotera

2011

Phys. Rev. D

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Newly born magnetars are good candidate sources of ultrahigh energy cosmic rays. These objects can in principle easily accelerate particles to the highest energies required to satisfy the ultrahigh energy cosmic ray scenario (E ∼ 10 20−21 eV), thanks to their important rotational and magnetic energy reservoirs. Their acceleration mechanism, based on unipolar induction, predicts however a hard particle injection that does not fit the observed ultrahigh energy cosmic ray spectrum. Here we show that an adequate distribution of initial voltages among magnetar winds can be found to soften the spectrum. We discuss the effect of these distributions for the stochastic gravitational wave background signature produced by magnetars. The magnetar population characteristics needed to fit the ultrahigh energy cosmic ray spectrum could lead in most optimistic cases to gravitational wave background signals enhanced of up to four orders of magnitudes in the range of frequency 1 − 100 Hz, compared to the standard predictions. These signals could reach the sensitivities of future detectors such as DECIGO or BBO.

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The birthrate of magnetars

Cited by 38 publications

References 37 publications

Quark-nova remnants

Quark-nova remnants

Population synthesis studies of isolated neutron stars with magnetic field decay

Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures

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