Magnetar-Like Activity From the Central Compact Object in the SNR Rcw103

Rea, N.; Borghese, A.; Esposito, P.; Zelati, F. Coti; Bachetti, Matteo; Israel, G. L.; Luca, A. De

doi:10.3847/2041-8205/828/1/l13

Cited by 103 publications

(127 citation statements)

References 44 publications

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“…It also means that the persistent X-ray luminosity and outburst of the super-slow magnetar originate from the magnetic energy. The outburst of the super-slow magnetar indeed resemble those of typical magnetars (Rea & Esposito 2011;D'Ai et al 2016;Rea et al 2016). Though the disk activity has faded away, the magnetic dipole field is not expected to decay significantly in 2 kyr (Vigano et al 2013).…”

Section: Calculation For the Super-slow Magnetar In Rcw 103mentioning

confidence: 75%

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Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Tong¹,

Wang²,

Liu³

et al. 2016

ApJ

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Magnetars may have strong surface dipole field. Observationally, two magnetars may have passive fallback disks. In the presence of a fallback disk, the rotational evolution of magnetars may be changed. In the self-similar fallback disk model, it is found that: (1) When the disk mass is significantly smaller than 10 −6 M ⊙ , the magnetar is unaffected by the fallback disk and it will be a normal magnetar. (2) When the disk mass is large, but the magnetar's surface dipole field is about or below 10 14 G, the magnetar will also be a normal magnetar. A magnetar plus a passive fallback disk system is expected. This may correspond to the observations of magnetars 4U 0142+61, and 1E 2259+586. (3) When the disk mass is large, and the magnetar's surface dipole field is as high as 4 × 10 15 G, the magnetar will evolve from the ejector phase to the propeller phase, and then enter rotational equilibrium. The magnetar will be slowed down quickly in the propeller phase. The final rotational period can be as high 2 × 10 4 s. This may correspond to the super-slow magnetar in the supernova remnant RCW 103. Therefore, the three kinds of magnetars can be understood in a unified way.

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Section: Calculation For the Super-slow Magnetar In Rcw 103mentioning

confidence: 75%

“…Recently, the central compact object (CCO) in supernova remnant RCW 103 is found to be a magnetar (D'Ai et al 2016;Rea et al 2016). The magnetar-like burst, outburst, and transient hard X-ray emissions all resemble those of classical magnetars (Rea & Esposito 2011).…”

Section: Introductionmentioning

confidence: 99%

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Tong¹,

Wang²,

Liu³

et al. 2016

ApJ

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“…Thus it is likely that 1E 161348−5055 also possesses a magnetic field in this range, and hereafter we will assume this is the case. While B may be similar to other magnetars, the 6.67 hr period of 1E 161348−5055 (which we will assume is its spin period; see D 'Aì et al 2016;Rea et al 2016) is drastically longer than the spin period of other magnetars, which are all in the range 2 − 12 s. Furthermore, this long period of 1E 161348−5055 could be used to argue against the generation of magnetar-strength magnetic fields via a dynamo mechanism, since this mechanism requires an inic 2016 The Authors tial rapid (possibly millisecond) spin period (Thompson & Duncan 1993;Bonanno et al 2005;Spruit 2009;Ferrario et al 2015).…”

Section: Introductionmentioning

confidence: 93%

“…The recent detection by D' Aì et al (2016); Rea et al (2016) of high energy activity from the neutron star (NS) 1E 161348−5055 in supernova remnant RCW 103 (also known as SNR G332.4−0.4) finally provides insights into its perplexing nature. Tuohy & Garmire (1980) discovered the X-ray point source 1E 161348−5055 using Einstein, but no corresponding optical/IR or radio counterpart has been found to date (Tuohy et al 1983;, which argues in part against the source being in a binary system.…”

Section: Introductionmentioning

confidence: 99%

Ejector and propeller spin-down: how might a superluminous supernova millisecond magnetar become the 6.67 h pulsar in RCW 103

Andersson

2016

Monthly Notices of the Royal Astronomical Society: Letters

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The X-ray source 1E 161348−5055 in the supernova remnant RCW 103 recently exhibited X-ray activity typical of magnetars, i.e. neutron stars with magnetic fields 10 14 − 10 15 G. However, 1E 161348−5055 has an observed period of 6.67 hr, in contrast to magnetars which have a spin period of seconds. Here we describe a simple model which can explain the spin evolution of 1E 161348−5055, as well as other magnetars, from an initial period of milliseconds that would be required for dynamo generation of magnetar-strength magnetic fields. We propose that the key difference between 1E 161348−5055 and other magnetars is the persistence of a remnant disk of small total mass. This disk caused 1E 161348−5055 to undergo ejector and propeller phases in its life, during which strong torques caused a rapid increase of its spin period. By matching its observed spin period and ≈ 1 − 3 kyr age, we find that 1E 161348−5055 has the (slightly) highest magnetic field of all known magnetars, with B ∼ 5 × 10 15 G, and that its disk had a mass of ∼ 10 24 g, comparable to that of the asteroid Ceres.

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“…Earlier jets could have had different directions, like precessing jets, and hence the arcs have Meaburn et al 1996), and NGC 3918 (both images are from Corradi et al 1999; images are rotated so that the jets are vertical). The image of RCW 103 is a composite X-ray image in three energy bands (low=red, medium=green, highest=blue) combined with an optical image from the Digitized Sky Survey (image taken from the Chandra website based on Rea et al 2016). The proposed original directions of the, already dead, jets in the CCSNR RCW 103 are marked by yellow thick arrows.…”

Section: Rcw 103mentioning

confidence: 99%

The imprints of the last jets in core collapse supernovae

Bear

Grichener²,

Soker

2017

Monthly Notices of the Royal Astronomical Society

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We analyze the morphologies of three core collapse supernova remnants (CCSNRs) and the energy of jets in other CCSNRs and in Super Luminous Supernovae (SLSNe) of type Ib/Ic/IIb, and conclude that these properties are well explained by the last jets' episode as expected in the jet feedback explosion mechanism of core collapse supernovae (CCSNe). The presence of two opposite protrusions, termed ears, and our comparison of the CCSNR morphologies with morphologies of planetary nebulae strengthen the claim that jets play a major role in the explosion mechanism of CCSNe. We crudely estimate the energy that was required to inflate the ears in two CCSNRs, and assume that the ears were inflated by jets. We find that the energies of the jets that inflated ears in 11 CCSNRs span a range that is similar to that of jets in some energetic CCSNe (SLSNe), and that this energy, only of the last jets' episode, is much less than the explosion energy. This finding is compatible with the jet feedback explosion mechanism of CCSNe, where only the last jets, that carry a small fraction of the total energy carried by earlier jets, are expected to influence the outer parts of the ejecta. We reiterate our call for a paradigm shift from neutrino-driven to jet-driven explosion models of CCSNe.

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Magnetar-Like Activity From the Central Compact Object in the SNR Rcw103

Cited by 103 publications

References 44 publications

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Rotational Evolution of Magnetars in the Presence of a Fallback Disk

Ejector and propeller spin-down: how might a superluminous supernova millisecond magnetar become the 6.67 h pulsar in RCW 103

The imprints of the last jets in core collapse supernovae

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