A double-sided radio jet from the compact Galactic Centre annihilator 1E1740.7–2942

Mirabel, I. F.; Rodrı́guez, Luis F.; Cordier, B.; Paul, J.; Lebrun, F.

doi:10.1038/358215a0

Cited by 420 publications

(297 citation statements)

References 7 publications

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“…It has been suggested that this source is powered by Bondi-Hoyle accretion from the cloud onto a compact object, such as a stellar mass black hole (Bally and Leventhal, 1991;Sunyaev et al, 1991). Phillips, Lazio, and Joseph (1995) found a 15Љ offset between HCO ϩ emission and the radio continuum hotspots which are used to locate the compact object Mirabel et al, 1992). They suggested that the offset occurs because of enhanced destruction or reduced formation of HCO ϩ in the x-ray field near the compact object, a suggestion confirmed by XDR models (Lepp and Dalgarno, 1996;Yan and Dalgarno, 1997).…”

Section: B X-ray Dissociation Regionsmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

736

712

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The interstellar medium of galaxies is the reservoir out of which stars are born and into which stars inject newly created elements as they age. The physical properties of the interstellar medium are governed in part by the radiation emitted by these stars. Far-ultraviolet (6 eVϽh Ͻ13.6 eV) photons from massive stars dominate the heating and influence the chemistry of the neutral atomic gas and much of the molecular gas in galaxies. Predominantly neutral regions of the interstellar medium in which the heating and chemistry are regulated by far ultraviolet photons are termed PhotoDissociation Regions (PDRs). These regions are the origin of most of the non-stellar infrared (IR) and the millimeter and submillimeter CO emission from galaxies. The importance of PDRs has become increasingly apparent with advances in IR and submillimeter astronomy. The IR emission from PDRs includes fine structure lines of C, C ϩ , and O; rovibrational lines of H 2 ; rotational lines of CO; broad mid-IR features of polycyclic aromatic hydrocarbons; and a luminous underlying IR continuum from interstellar dust. The transition of H to H 2 and C ϩ to CO occurs within PDRs. Comparison of observations with theoretical models of PDRs enables one to determine the density and temperature structure, the elemental abundances, the level of ionization, and the radiation field. PDR models have been applied to interstellar clouds near massive stars, planetary nebulae, red giant outflows, photoevaporating planetary disks around newly formed stars, diffuse clouds, the neutral intercloud medium, and molecular clouds in the interstellar radiation field-in summary, much of the interstellar medium in galaxies. Theoretical PDR models explain the observed correlations of the [CII] 158 m with the CO Jϭ1 -0 emission, the CO Jϭ1 -0 luminosity with the interstellar molecular mass, and the [CII] 158 m plus [OI] 63 m luminosity with the IR continuum luminosity. On a more global scale, PDR models predict the existence of two stable neutral phases of the interstellar medium, elucidate the formation and destruction of star-forming molecular clouds, and suggest radiation-induced feedback mechanisms that may regulate star formation rates and the column density of gas through giant molecular clouds. [S0034-6861(99)01001-6] CONTENTS

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Section: B X-ray Dissociation Regionsmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

736

712

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“…A different explanation of the redshift, assuming positron annihilation, is that the observed ∼0.4 MeV line energy is due to the motion of the annihilating region (Misra and Melia 1993) where the pairs annihilate at the base of a jet emanating from the black hole. This explanation would allow the separation of the annihilation region from the pair production region.…”

Section: Line Features From Black Hole Candidatesmentioning

confidence: 99%

“…Skibo, private communication 1994), essentially the same as that for the backscatter model, so that the implied black hole mass is nearly identical. Also radio observations show that 1E1740.7-2942 is in fact associated with a double sided jet (Mirabel et al 1992). …”

Section: Line Features From Black Hole Candidatesmentioning

confidence: 99%

“…It was shown that cosmic rays with flux equal to the observed flux near Earth, interacting with interstellar matter prior to the formation of the solar system, can produce the observed solar system abundances of 6 Li, 9 Be and 10 B (Meneguzzi, Audouze and Reeves 1971;Mitler 1972). Since low energy cosmic rays with spectra similar to that of the accelerated particles in Orion also produce these isotopes, the Galactic inventories of 6 Li, 9 Be and 10 B can set limits on the total Galactic irradiation by such low energy cosmic rays.…”

Section: The Relationship To Light Isotope Productionmentioning

confidence: 99%

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Astrophysical Gamma Ray Emission Lines

Ramaty¹,

Lingenfelter²

1995

The Analysis of Emission Lines

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We review the wide range of astrophysical observations of gamma ray emission lines and we discuss their implications. We consider line emission from solar flares, the Orion molecular cloud complex, supernovae 1987A and 1991T, the supernova remnants Cas A and Vela, the interstellar medium, the Galactic center region and several Galactic black hole candidates. The observations have important, and often unique, implications on particle acceleration, star formation, processes of nucleosynthesis, Galactic evolution and compact object physics.

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“…These sources are called microquasars [128] [129], exploiting an analogy discussed in more detail below. Figure 2, from [130], is a sketch of an X-ray binary, presenting the major physical components and sites of emission in such systems.…”

Section: Microquasars and Jetsmentioning

confidence: 99%

Atomic X-ray spectroscopy of accreting black holes

Liedahl¹,

Torres²

2005

Can. J. Phys.

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Current astrophysical research suggests that the most persistently luminous objects in the Universe are powered by the flow of matter through accretion disks onto black holes. Accretion disk systems are observed to emit copious radiation across the electromagnetic spectrum, each energy band providing access to rather distinct regimes of physical conditions and geometric scale. X-ray emission probes the innermost regions of the accretion disk, where relativistic effects prevail. While this has been known for decades, it also has been acknowledged that inferring physical conditions in the relativistic regime from the behavior of the X-ray continuum is problematic and not satisfactorily constraining. With the discovery in the 1990s of iron X-ray lines bearing signatures of relativistic distortion came the hope that such emission would more firmly constrain models of disk accretion near black holes, as well as provide observational criteria by which to test general relativity in the strong field limit. Here we provide an introduction to this phenomenon. While the presentation is intended to be primarily tutorial in nature, we aim also to acquaint the reader with trends in current research. To achieve these ends, we present the basic applications of general relativity that pertain to X-ray spectroscopic observations of black hole accretion disk systems, focusing on the Schwarzschild and Kerr solutions to the Einstein field equations. To this we add treatments of the fundamental concepts associated with the theoretical and modeling aspects of accretion disks, as well as relevant topics from observational and theoretical X-ray spectroscopy. PACS Nos.: 32.30. Rj, 32.80.Hd, 95.30.Dr, 95.30.Sf, 95.85.Nv, 97.10.Gz. 97.80.Jp, 98.35.Mp, 98.62.Mw

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A double-sided radio jet from the compact Galactic Centre annihilator 1E1740.7–2942

Cited by 420 publications

References 7 publications

Photodissociation regions in the interstellar medium of galaxies

Photodissociation regions in the interstellar medium of galaxies

Astrophysical Gamma Ray Emission Lines

Atomic X-ray spectroscopy of accreting black holes

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