Frontiers of Astrophysics—Workshop summary

Biermann, Peter L.; Falcke, H.

doi:10.1063/1.55085

Cited by 6 publications

(9 citation statements)

References 116 publications

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“…Furthermore, the remnant is detected with the Very Large Array (VLA) at 1.49 & 4.86 GHz as a nonthermal, polarized radio source with a spectral index of -0.67 and a flux of 24 mJy at 1 GHz (Reynolds & Chevalier 1984). In addition, the flux densities are 8.7, 20.6, 29, 33 and 38 mJy at frequencies 4.86, 1.49, 0.608, 0.408 and 0.327 GHz, respectively (Biermann, Strom, & Falcke 1995). This shows the existence of shocked circumstellar or interstellar material.…”

Section: Introductionmentioning

confidence: 99%

ChandraObservation of the Shell of Nova Persei 1901 (GK Persei): Detection of Localized Nonthermal X‐Ray Emission from a Miniature Supernova Remnant

Balman

2005

ApJ

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I present the data of the shell of classical Nova Persei (1901) obtained by the Advanced CCD Imaging Spectrometer S3 detector on-board Chandra Observatory. The X-ray nebula is affected mostly by the complex interstellar medium around the nova and has not developed a regular shell. The X-ray nebula is lumpy and asymmetric with bulk of emission coming from the southwestern quadrant. The brightest X-ray emission is detected as an arc that covers from the west to the south of the central source. Part of this feature, which is co-spatial with the brightest non-thermal radio emission region, is found to be a source of nonthermal (synchrotron) X-ray emission with a power law photon index of 2.3 +1.5 −0.9 and α=0.68 +0.03 −0.15 at about a flux of 1.7×10 −13 erg cm −2 s −1 . This confirms that the shell is a cite of particle acceleration, mainly in the reverse shock zone. There are strong indications for nonlinear diffusive shock acceleration occurring in the forward shock/transition zone with an upper limit on the non-thermal X-ray flux of 1.0×10 −14 erg cm −2 s −1 . The total X-ray spectrum of the nebula consists of two prominent components of emission (other than the resolved synchrotron X-ray emission). The component dominant below 2 keV is most likely a nonequilibrium ionization thermal plasma of kT s =0.1-0.3 keV with an X-ray flux of 1.6×10 −11 erg cm −2 s −1 . There is also a higher temperature, kT s =0.5-2.6 keV, embedded, N H =(4.0-22.0)×10 22 cm −2 , emission component prominent above 2 keV. The unabsorbed X-ray flux from this component is 1.5×10 −10 erg cm −2 s −1 . The X-ray emitting plasma is of solar composition except for enhancement in the elemental abundances (mean abundances over the remnant) of Ne/Ne ⊙ and N/N ⊙ in a range 13-21 and 1-5, respectively. A distinct emission line of neon, He-like Ne IX, is detected which reveals a distribution of several emission knots/blobs and shows a cone-like structure with wings extending toward NW and SE at expansion velocities about 2600 km s −1 in the X-ray wavelengths.The emission measures yield an average electron density in a range 0.6-11.2 cm −3 for both of the components (filling factor=1). The electron density increases to higher values ∼ 300 cm −3 if the filling factor is decreased substantially. The mass in the X-ray emitting nebula is (2.1-38.5)×10 −4 M ⊙ . The X-ray luminosity of the forward shock ∼ 4.3×10 32 erg s −1 indicates that it is adiabatic. The shocked mass, the X-ray luminosity and comparisons with other wavelengths suggest that the remnant has started cooling and most likely is in a Sedov phase.

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Section: Introductionmentioning

confidence: 99%

ChandraObservation of the Shell of Nova Persei 1901 (GK Persei): Detection of Localized Nonthermal X‐Ray Emission from a Miniature Supernova Remnant

Balman

2005

ApJ

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“…iv) The low-energy cutoff in the energetic electron spectra of the jets suggested by the radio spectra [17] is conveniently explained by the pion decay resulting from proton-proton collisions [18]. The latter mechanism require a relativistic temperature in the accretion disk near the foot of the jet, which translates to the central black hole spinning extremely fast [19].…”

Section: Introductionmentioning

confidence: 99%

Spinning compact binary inspiral. II. Conservative angular dynamics

Gergely¹

2010

Phys. Rev. D

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We establish the evolution equations of the set of independent variables characterizing the 2PN rigorous conservative dynamics of a spinning compact binary, with the inclusion of the leading order spin-orbit, spin-spin and mass quadrupole -mass monopole effects, for generic (noncircular, nonspherical) orbits. More specifically, we give a closed system of first order ordinary differential equations for the orbital elements of the osculating ellipse and for the angles characterizing the spin orientations with respect to the osculating orbit.We also prove that (i) the relative angle of the spins stays constant for equal mass black holes, irrespective of their orientation, and (ii) the special configuration of equal mass black holes with equal, but antialigned spins, both laying in the plane of motion (leading to the largest recoil found in numerical simulations) is preserved at 2PN level of accuracy, with leading order spin-orbit, spin-spin and mass quadrupolar contributions included.

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“…The model for cosmic rays using a more detailed view of the stars that explode, by invoking the magnetic stellar wind, was developed quantitatively by Biermann et al Biermann and Cassinelli, 1993;Biermann and Strom, 1993;Stanev et al, 1993), then developed further in Biermann et al (1995Biermann et al ( , 2001, WiebelSooth et al (1998), and in . The new tests began with accounting for the cosmic-ray positrons and electrons , then for the high-frequency radio emission excess near the Galactic Center (called the WMAP excess) as well as the 511 keV annihilation emission also near the Galactic Center .…”

Section: Extragalactic and Galactic High Energy Particlesmentioning

confidence: 98%

From Ultra Rays to Astroparticles

Falkenburg¹,

Rhode²

2012

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Frontiers of Astrophysics—Workshop summary

Cited by 6 publications

References 116 publications

ChandraObservation of the Shell of Nova Persei 1901 (GK Persei): Detection of Localized Nonthermal X‐Ray Emission from a Miniature Supernova Remnant

ChandraObservation of the Shell of Nova Persei 1901 (GK Persei): Detection of Localized Nonthermal X‐Ray Emission from a Miniature Supernova Remnant

Spinning compact binary inspiral. II. Conservative angular dynamics

From Ultra Rays to Astroparticles

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