A Thorough Investigation of the Distance to the Supernova Remnant Ctb109 and Its Pulsar Axp J2301+5852

Kothes, R.; Foster, Tyler

doi:10.1088/2041-8205/746/1/l4

Cited by 47 publications

(60 citation statements)

References 24 publications

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“…which is much larger than the observed X-ray luminosity, L X = 1.8 × 10 34 erg s −1 , assuming a distance of 3.2 ± 0.2 kpc (Kothes & Foster 2012). The surface magnetic field of 1E 2259+586 inferred from Eq.…”

Section: Rotation Power and Magnetic Fieldmentioning

confidence: 65%

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

Boshkayev

Izzo

Rueda

et al. 2013

A&A

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Aims. We describe the so-called low magnetic field magnetars, SGR 0418+5729, Swift J1822.3-1606, and the AXP prototype 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs. Methods. We give bounds for the mass, radius, moment of inertia, and magnetic field for these sources by requesting the stability of realistic, general relativistic, uniformly rotating white dwarfs. We also present the theoretical expectation of the infrared, optical, and ultraviolet emission of these objects and show their consistency with the current available observational data. Results. We improve the theoretical prediction of the lower limit of the spindown rate of SGR 0418+5729; for a white dwarf close to its maximum stable mass we obtain the very stringent interval for the spindown rate of 4.1 × 10 −16 <Ṗ < 6 × 10 −15 , where the upper value is the known observational limit. A lower limit has been also set for Swift J1822.3-1606, whose spindown rate is not yet fully confirmed. Our model provides for the sourceṖ ≥ 2.13 × 10 −15 if the star is close to its maximum stable mass. We give in addition the frequencies at which absorption features could be present in the spectrum of these sources as the result of the scattering of photons with the quantized electrons by the surface magnetic field.Key words. stars: magnetic field -stars: rotation -white dwarfs -stars: magnetars IntroductionSoft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are a class of compact objects that show interesting observational properties (see, e.g., Mereghetti 2008): rotational periods in the range P ∼ (2−12) s, spindown ratesṖ ∼ (10 −13 -10 −10 ), strong outburst of energies ∼(10 41 −10 43 ) erg, and in the case of SGRs, giant flares of even large energies ∼(10 44 -10 47 ) erg.The most popular model for the description of SGRs and AXPs, the magnetar model, is based on a neutron star of fiducial parameters M = 1.4 M , R = 10 km, and a moment of inertia I = 10 45 g cm 2 . It needs a neutron star magnetic field larger than the critical field for vacuum polarization B c = m 2 e c 3 /(e ) = 4.4 × 10 13 G in order to explain the observed X-ray luminosity in terms of the release of magnetic energy (Duncan & Thompson 1992; Thompson & Duncan 1995). There exist in the literature other models still based on neutron stars but of ordinary fields B ∼ 10 12 G; these models involve either the generation of drift waves in the magnetosphere or the accretion of fallback material via a circumstellar disk (see Malov 2010;Trümper et al. 2013, respectively, and references therein).Turning to the experimental point of view, the observation of SGR 0418+5729 with a rotational period of P = 9.08 s, an upper limit of the first time derivative of the rotational perioḋ P < 6.0 × 10 −15 (Rea et al. 2010), and an X-ray luminosity of L X = 6.2 × 10 31 erg s −1 can be considered as the Rosetta Stone for alternative models of SGRs and AXPs. The inferred upper limit of the surface magnetic field of SGR 0418+5729, B < 7.5 × 10 12 G; which describes it as a neutr...

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Section: Rotation Power and Magnetic Fieldmentioning

confidence: 65%

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

Boshkayev

Izzo

Rueda

et al. 2013

A&A

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“…The obtained spectra of the shell and the Lobe could be well fitted with a one-component non-equilibrium ionisation (NEI) model, describing a mixture of the shocked ISM and shocked ejecta. The preshock density of the ambient medium was derived to be n 0 = (0.16 ± 0.02) d −0.5 3 cm −3 , where d 3 = D/3.0 kpc is a scaling factor accounting for the distance D of CTB 109, which was estimated as 3.2 ± 0.2 kpc by Kothes & Foster (2012) with the new method of Foster & MacWilliams (2006). This results in a density of the medium of n 0 = 0.155 cm −3 in case of the XMM-Newton data.…”

Section: Model Setupmentioning

confidence: 99%

“…Recent measurements show that the distance to CTB 109 lies between 3 and 4 kpc (Kothes et al 2002;Tian et al 2010); the latest value is 3.2 ± 0.2 kpc (Kothes & Foster 2012). It is even more difficult to determine the proper motion of A&A 582, A47 (2015) (Kothes et al 2002) from the Canadian Galactic Plane Survey (CGPS, Taylor et al 2003).…”

Section: Introductionmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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Context. Using detailed 3D hydrodynamic simulations we study the nature of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well known for its semicircular shape and a bright diffuse X-ray emission feature inside the SNR. Aims. Our model has been designed to explain the observed morphology, with a special emphasis on the bright emission feature inside the SNR. Moreover, we determine the age of the remnant and compare our findings with X-ray observations. With CTB 109 we test a new method of detailed numerical simulations of diffuse young objects, using realistic initial conditions derived directly from observations. Methods. We performed numerical 3D simulations with the RAMSES code. The initial density structure has been directly taken from 12 CO emission data, adding an additional dense cloud, which, when it is shocked, causes the bright emission feature.Results. From parameter studies we obtained the position ( , b) = (109.1545 • , −1.0078 • ) for an elliptical cloud with n cloud = 25 cm −3 based on the preshock density from Chandra data and a maximum diameter of 4.54 pc, whose encounter with the supernova (SN) shock wave generates the bright X-ray emission inside the SNR. The calculated age of the remnant is about 11 000 yr according to our simulations. In addition, we can also determine the most probable site of the SN explosion. Conclusions. Hydrodynamic simulations can reproduce the morphology and the observed size of the SNR CTB 109 remarkably well. Moreover, the simulations show that it is very plausible that the bright X-ray emission inside the SNR is the result of an elliptical dense cloud shocked by the SN explosion wave. We show that numerical simulations using observational data for an initial model can produce meaningful results.

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“…A spiral shock in the Perseus arm is "pushing" objects, including H ii regions, SNRs, and PWNe, towards the Galactic centre, giving them -from our point of view -a higher negative radial velocity, which makes them appear to be farther away than they actually are (Roberts 1972). Examples of this effect on distance estimates of SNRs and PWNe can be found for instance in Kothes et al ( , 2003 and Foster et al (2004) and most recently in Kothes & Foster (2012). SNRs and PWNe in particular rely heavily on kinematic With permission of Crown Copyright 2013 NRC Canada.…”

Section: Introductionmentioning

confidence: 77%

Distance and age of the pulsar wind nebula 3C 58

Kothes¹

2013

A&A

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Context. A growing number of researchers present evidence that the pulsar wind nebula 3C 58 is much older than predicted by its proposed connection to the historical supernova of A.D. 1181. There is also a great diversity of arguments. The strongest of these arguments rely heavily on the assumed distance of 3.2 kpc determined with H i absorption measurements.Aims. This publication aims at determining a more accurate distance for 3C 58 and at re-evaluating the arguments for an older age.Methods. I have re-visited the distance determination of 3C 58 based on new H i data from the Canadian Galactic Plane Survey and our recent improvements in the knowledge of the rotation curve of the outer Milky Way Galaxy. I also used newly determined distances to objects in the neighbourhood, which are based on direct measurements by trigonometric parallax. Results. I have derived a new more reliable distance estimate of 2 kpc for 3C 58. This makes the connection between the pulsar wind nebula and the historical event from A.D. 1181 once again much more viable.

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A Thorough Investigation of the Distance to the Supernova Remnant Ctb109 and Its Pulsar Axp J2301+5852

Cited by 47 publications

References 24 publications

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Distance and age of the pulsar wind nebula 3C 58

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