An X-ray and optical study of the supernova remnant W44

Rho, Jeonghee; Petre, Robert; Schlegel, Eric M.; Hester, J. J.

doi:10.1086/174446

Cited by 83 publications

(135 citation statements)

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“…The result can be observed in the bottom right panel. Again, we have considered the complete photon energy range of 0.3-10 keV, but we have now included the extinction produced by the ISM for an H i column density of 1:8 Â 10 22 cm À2 (Rho et al 1994) in computing the X-ray emission map. For these calculations, we have considered the frequency-dependent extinction of Morrison & McCammon (1983).…”

Section: Expansion Into a Uniform Environmentmentioning

confidence: 99%

“…This high-resolution image shows an elongated shell of about 34 0 Â 24 0 in size, with numerous knots and filamentary arcs of synchrotron radiation, both in the interior and along the perimeter of W44. Figure 8 (right) shows the radio emission at 1.4 GHz (contours) superposed on a gray-scale representation of the ROSAT X-ray emission (taken from Rho et al 1994). The brightest soft X-ray emission is concentrated toward the center of the remnant, where it has a knotty and irregular distribution.…”

Section: W44mentioning

confidence: 99%

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Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Velázquez

Martinell

Raga

et al. 2004

ApJ

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Several physical mechanisms have been studied in order to explain why composite supernova remnants (SNRs) have shell-like morphologies in the radio continuum while their X-ray emission is centrally peaked. One of the proposed mechanisms has been the presence of thermal conduction, which can raise the density at the center of SNRs, increasing the X-ray emission from these regions. In this work, we have carried out axisymmetric numerical simulations with the adaptive grid Yguazú-a code, which includes advection of the magnetic field and thermal conduction. We have considered cases with anisotropic and isotropic thermal conduction, as well as with no conduction. We have simulated X-ray (as well as radio synchrotron) emission maps from our numerical simulations, which can be directly compared with observations.

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Section: Expansion Into a Uniform Environmentmentioning

confidence: 99%

Section: W44mentioning

confidence: 99%

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Velázquez

Martinell

Raga

et al. 2004

ApJ

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“…This is in contrast to the radio morphology which is more shelllike. This suggests that G290.1−0.8 is like the supernova remnant W44 (Rho et al 1994), which, like W28 and 3C400.2 (Long et al 1991), has centrally peaked X-ray emission but shell-like radio morphology. The central X-ray emission in these remnants is thermal.…”

Section: Observations and Resultsmentioning

confidence: 97%

“…Milne et al (1989) estimated the remnant to be only 2.2 kyr old, assuming the smallest distance estimate. Rho (1995) suggests the remnant is somewhat older, ∼10 kyr. The resemblance of the optical emission to that of the Monoceros Ring, whose age is ∼ 50 kyr (Leahy, Naranan, & Singh 1986), suggests a much larger age for G290.1−0.8.…”

Section: Observations and Resultsmentioning

confidence: 99%

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Discovery of the young, energetic radio pulsar PSR J1105−6107

Kaspi¹,

Bailes²,

Manchester³

et al. 1997

AIP Conference Proceedings

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We report the discovery and follow-up timing observations of the 63 ms radio pulsar, PSR J1105−6107. The pulsar is young, having a characteristic age of only 63 kyr and, from its dispersion measure, is estimated to be at a distance of ∼7 kpc from the Sun. We consider its possible association with the nearby supernova remnant G290.1−0.8 (MSH 11−61A); an association requires that the pulsar's proper motion be ∼22 mas yr −1 (corresponding to ∼650 km s −1 for a distance of 7 kpc) directed away from the remnant center, assuming that the characteristic age is the true age. The pulsar's spin-down luminosity, 2.5×10 36 erg s −1 , is in the 1 Hubble Fellow 2 Current address: Kvednaberget 12, 4033 Forus, Norway -2 -top 1% of all known pulsar spin-down luminosities. Given its estimated distance, PSR J1105−6107 is therefore likely to be observable at high energies. Indeed, it is coincident with the known CGRO/EGRET source 2EG J1103−6106; we consider the possible association and conclude that it is likely.

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The origin of Cosmic-Rays from SNRs: confirmations and challenges after the first direct proof

Cardillo

Tavani

Giuliani

2014

Nuclear Physics B - Proceedings Supplements

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Until now, providing an experimental unambiguous proof of Cosmic Ray (CR) origin has been elusive. The SuperNova Remnant (SNR) study showed an increasingly complex scenario with a continuous elaboration of theoretical models. The middle-aged supernova remnant (SNR) W44 has recently attracted attention because of its relevance regarding the origin of Galactic cosmicrays. The gamma-ray missions AGILE and Fermi have established, for the first time for a SNR, the spectral continuum below 200 MeV which can be attributed to neutral pion emission. Our work is focused on a global re-assessment of all available data and models of particle acceleration in W44 and our analysis strengthens previous studies and observations of the W44 complex environment, providing new information for a more detailed modeling. However, having determined the hadronic nature of the gamma-ray emission on firm ground, a number of theoretical challenges remains to be addressed in the context of CR acceleration in SNRs.

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An X-ray and optical study of the supernova remnant W44

Cited by 83 publications

References 0 publications

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Effects of Thermal Conduction on the X‐Ray and Synchrotron Emission from Supernova Remnants

Discovery of the young, energetic radio pulsar PSR J1105−6107

The origin of Cosmic-Rays from SNRs: confirmations and challenges after the first direct proof

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