Far-Ultraviolet Observations of the Monogem Ring

Ij, Kim; Kang, Min; Seon, Kwang‐Il; Jw, Park; Han, Wonyong; Jh, Park; Nam, UW; Edelstein, Jerry; Sankrit, Ravi; Korpela, E. J.

doi:10.1086/521441

Cited by 15 publications

(14 citation statements)

References 18 publications

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“…we have developed several programs in C and FORTRAN in order to obtain results presented in this paper. The area of Monoceros loop is very difficult to determine precisely due to great influence of background radiation and superposed external sources, such as Rosette Nebula (Graham et al 1982;Aharonian et al 2004Aharonian et al , 2007Kim et al 2007). Therefore, some authors made very rough estimates for the shape of this loop, representing it by fitted circles (see e.g.…”

Section: Methodsmentioning

confidence: 99%

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The Monoceros radio loop: Temperature, brightness, spectral index, and distance

Jovanović¹,

Urošević

2009

Astron Nachr

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In this paper we estimated the temperatures and brightnesses of the Monoceros radio loop at 1420, 820 and 408 MHz. The linear spectrum is estimated for mean temperatures versus frequency between 1420, 820 and 408 MHz. The spectral index of Monoceros loop is also obtained. The brightness temperatures and surface brightnesses of the loop are computed using data taken from radio‐continuum surveys at the three frequencies. The spectral index of the loop is also obtained from T‐T plots between 1420–820, 1420–408, and 820–408 MHz. The obtained results confirm non‐thermal origin of the Monoceros radio loop (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Section: Methodsmentioning

confidence: 99%

“…Therefore, some authors made very rough estimates for the shape of this loop, representing it by fitted circles (see e.g. Aharonian et al 2004;Kim et al 2007). In order to make better estimates for the loop boundaries, we analyzed temperature profiles (see Fig.…”

Section: Methodsmentioning

confidence: 99%

The Monoceros radio loop: Temperature, brightness, spectral index, and distance

Jovanović¹,

Urošević

2009

Astron Nachr

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“…It is also possible that Geminga is running into an unrelated turbulent region at present. Kim et al (2007) discovered a large ring-like structure in Hα emission that is centered at (97.14 • , 21.33 • ) in equatorial coordinates, dubbed the 'Gemini Hα Ring'. As can be seen in Figure 5, the most intense part of the Geminga TeV halo is included by the Gemini Hα Ring in projection.…”

Section: Is Geminga Inside a Stellar-wind Bubble?mentioning

confidence: 99%

“…As can be seen in Figure 5, the most intense part of the Geminga TeV halo is included by the Gemini Hα Ring in projection. There is evidence that the Gemini Hα Ring is interacting with the Monogem Ring (Kim et al 2007). As the distance of Monogem Ring is estimated to be ∼ 300 pc (Knies et al 2018), the Gemini Hα Ring should have a similar distance.…”

Section: Is Geminga Inside a Stellar-wind Bubble?mentioning

confidence: 99%

Possible origin of the slow-diffusion region around Geminga

Fang

Yin

2019

Monthly Notices of the Royal Astronomical Society

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Geminga pulsar is surrounded by a multi-TeV γ-ray halo radiated by the high energy electrons and positrons accelerated by the central pulsar wind nebula (PWN). The angular profile of the γ-ray emission reported by HAWC indicates an anomalously slow diffusion for the cosmic-ray electrons and positrons in the halo region around Geminga. In the paper we study the possible mechanism for the origin of the slow diffusion. At first, we consider the self-generated Alfvén waves due to the streaming instability of the electrons and positrons released by Geminga. However, even considering a very optimistic scenario for the wave growth, we find this mechanism DOES NOT work to account for the extremely slow diffusion at the present day if taking the proper motion of Geminga pulsar into account. The reason is straightforward as the PWN is too weak to generate enough high energy electrons and positrons to stimulate strong turbulence at the late time. We then propose an assumption that the strong turbulence is generated by the shock wave of the parent supernova remnant (SNR) of Geminga. Geminga may still be inside the SNR, and we find that the SNR can provide enough energy to generate the slow-diffusion circumstance. The TeV halos around PSR B0656+14, Vela X, and PSR J1826-1334 may also be explained under this assumption.

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“…As a result, models for such bubbles have not been able to explain the soft X‐ray emission observed by McCammon et al (1983). Nor can they explain the emissivity in high‐stage ions, such as O vi , N v , C iv and Si iv (Blair, Sankrit & Tulin 2002; Shinn et al 2006; Kim et al 2007; Park et al 2007). Explaining such emission requires gas in the range spanning 3 × 10 5 K to a few ×10 6 K, with the O vi data favouring the lower part of that temperature range and the soft X‐ray data favouring the higher part of that range.…”

Section: Introductionmentioning

confidence: 99%

Simulating anisotropic thermal conduction in supernova remnants – II. Implications for the interstellar medium

Balsara

Bendinelli

Tilley

et al. 2008

Monthly Notices RAS

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We present a large number of 2.5D simulations of supernova remnants expanding into interstellar media having a range of densities, temperatures and magnetic field strengths. The simulations include equilibrium cooling and anisotropic, flux-limited thermal conduction along magnetic field lines. The volume of hot gas produced during the remnant's evolution is shown to be strongly influenced by the inclusion of thermal conduction, supporting prior results by Slavin & Cox and Tilley & Balsara. The magnetic field has also been shown to play an extremely important role in reheating the gas at later epochs when the hot gas bubble collapses on itself. Low-density, strongly magnetized runs show the greatest effect of this reheating.The four-volumes and three-areas of gas with characteristic temperatures that cause it to emit in O VI, O VII and O VIII have also been catalogued and their dependence on interstellar parameters has been documented. The results reveal the importance of magnetic tension forces as well as the anisotropic thermal conduction along field lines for the production of these ions. Simulated luminosities and linewidths of O VI, O VII and O VIII as well as their dosages have been catalogued.Simulated linewidths of radioactive species, 26 Al and 60 Fe, ejected by supernovae have also been catalogued and found to be less than 200 km s −1 for most of the remnants' evolution. These results enable us to understand why INTEGRAL has thus far been unable to detect very large linewidths for these radioactive species in certain star-forming regions.

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Far-Ultraviolet Observations of the Monogem Ring

Cited by 15 publications

References 18 publications

The Monoceros radio loop: Temperature, brightness, spectral index, and distance

The Monoceros radio loop: Temperature, brightness, spectral index, and distance

Possible origin of the slow-diffusion region around Geminga

Simulating anisotropic thermal conduction in supernova remnants – II. Implications for the interstellar medium

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