The interacting subsystems theory of active galactic nuclei -- I. The broad-absorption-line QSO theory

Vilkoviskij, E. Y.; Efimov, S. N.; Karpova, O. G.; Павлова, Л. А.

doi:10.1046/j.1365-8711.1999.02793.x

Cited by 17 publications

(17 citation statements)

References 40 publications

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“…S iv * λ1072.973 is not detected at z GRB ; we measure log N(S iv * ) < 13.70 (3σ) over the velocity range −25 to 20 km s −1 , in which we measure log N(S iv) = 14.61 ± 0.15, so that N(S iv * )/N(S iv) < 0.12. Note that this limit applies only to the strongest component of 5 Line-locking is understood as occurring when a cloud is accelerated by radiation pressure in a given doublet line until the wavelength shifts into the shadow of the other doublet line cast by a separate cloud (Vilkoviskij et al 1999). Note: the symbol * denotes a saturated component; no reliable column density or line width can be extracted for the component, and the total column density in that ion is uncertain.…”

Section: Grb 050730 Z Grb = 39686mentioning

confidence: 99%

High-ion absorption in seven GRB host galaxies at z = 2–4

Fox¹,

Ledoux²,

Vreeswijk

et al. 2008

A&A

118

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Aims. We use VLT/UVES high-resolution optical spectroscopy of seven GRB afterglows (at z GRB between 2.20 and 3.97) to investigate circumburst and interstellar plasma in the host galaxies of the bursts. Methods. GRBs 050730, 050820, 050922C, 060607, 071031, and 080310 were each detected by the Swift satellite. With the minimum possible time delay (as short as eight minutes), follow-up optical spectroscopy at 6.0 km s −1 resolution began with UVES. We present Voigt-profile component fits and analysis of the high-ion absorption detected in these spectra and in the pre-Swift UVES spectrum of GRB 021004, at velocities between z GRB -5000 km s −1 and z GRB . Results. We identify several distinct categories of high-ion absorption at velocities close to z GRB : (i) strong high-ion absorption at z GRB itself is always seen in O vi, C iv, and Si iv, usually (in six of seven cases) in N v, and occasionally in S iv and S vi. Three of the cases show log N(N v) > 14 in a single-component, suggesting a circumburst origin, but we cannot rule out an interstellar origin. Indeed, using the non-detection of S iv * at z GRB toward GRB 050730 together with a UV photo-excitation model, we place a lower limit of 400 pc on the distance of the S iv-bearing gas from the GRB; (ii) complex, multi-component C iv and Si iv profiles extending over 100-400 km s −1 around z GRB are observed in each spectrum; these velocity fields are similar to those measured in C iv in damped Lyman-α systems at similar redshifts, suggesting a galactic origin; (iii) asymmetric, blueshifted, absorption-line wings covering 65-140 km s −1 are seen in the C iv, Si iv, and O vi profiles in four of the seven GRB afterglow spectra. The wing kinematics together with the "Galactic" C iv/Si iv ratios measured in two cases suggest that the wings trace outflowing interstellar gas in the GRB host galaxies; (iv) high-velocity (HV; 500-5000 km s −1 relative to z GRB ) components are detected in six of the seven spectra; these components are not necessarily a single homogeneous population, and many of them may arise in unrelated foreground galaxies.However, in the cases of GRBs 071031 and 080310, the ionization properties of the HV components (very high C iv/Si iv ratios and absence of neutral-phase absorption in Si ii or C ii) are suggestive of a circumburst origin; models of Wolf-Rayet winds from the GRB progenitors can explain both the kinematics and ionization level of these HV components.

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Section: Grb 050730 Z Grb = 39686mentioning

confidence: 99%

High-ion absorption in seven GRB host galaxies at z = 2–4

Fox¹,

Ledoux²,

Vreeswijk

et al. 2008

A&A

118

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“…The high ionization is easily understood because of the intense UV flux of the QSO. The line-locking is explained as an effect of cloudlets being accelerated via absorption at a given transition until its wavelength falls into the shadow of another line in a cloud in front of it (Vilkoviskij et al 1999).…”

Section: The Nature Of the Grb Absorption Systemsmentioning

confidence: 99%

Absorption systems in the spectrum of GRB 021004

Møller

Fynbo

Hjorth

et al. 2002

A&A

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Abstract. We report on a 3600 s spectrum of GRB 021004 obtained with the Nordic Optical Telecope on La Palma 10.71 hours after the burst. We identify absorption lines from five systems at redshifts 1.3806, 1.6039, 2.2983, 2.3230, and 2.3292. In addition we find an emission line which, if due to Lyα from the host galaxy, gives a redshift of 2.3351. The nearest absorber is blueshifted by 530 km s −1 with respect to this line, consistent with shifts seen in Damped Lyα and Lyman-Break galaxies at similar redshifts. The emission line flux is 2.46 ± 0.50 × 10 −16 erg s −1 cm −2 . Some of the absorption systems are "line-locked", an effect often seen in QSO absorption systems believed to originate close to the QSO central engine.

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“…Our theoretical approach to the problem of matter outflow from AGN was presented in a series of papers by Vilkoviskij and Nosov (1994), Vilkoviskij, Karpova and Nosov (1996), , and in complete form by Vilkoviskij et al (1999;hereafter V99). Here, we recall the main points of this approach and discuss them in the light of new observational data.…”

Section: Interacting Subsystems Of Agns Evolution and Unification Scmentioning

confidence: 99%

“…Because of this the solution of the equation (1) can contain three critical points instead of one presented in the Parker solar wind equation . In this case the position of the trans-sonic point depends on the parameters of the equation; the most important parameter is the relation of the masses of the black hole and the CSC (Vilkoviskij et al, 1999).…”

Section: Unified Model Of the Absorbing Mass Outflowsmentioning

confidence: 99%

“…Thus equation (4) takes into account both the filling factor and the velocity of the clouds. A numerical code for solving the full system of equations described above has been developed by Vilkoviskij et al (1999). The solutions for the gas dynamics and resulting spectra were obtained under the following conditions: (i) The incoming AGN spectrum consists of Planck and power-low parts and includes the broad emission lines as well.…”

Section: Unified Model Of the Absorbing Mass Outflowsmentioning

confidence: 99%

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Matter Outflows from AGN: A Unifying Model

Vilkoviskij

Lovelace

Павлова

et al. 2006

Astrophys Space Sci

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We discuss a self-consistent unified model of the matter outflows from AGNs based on a theoretical approach and involving data on AGN evolution and structure. The model includes a unified geometry, two-phase gas dynamics, radiation transfer, and absorption spectrum calculations in the UV and X-ray bands. We briefly discuss several questions about the mass sources of the flows, the covering factors, and the stability of the narrow absorption details.Comment: 6 figures, accepted for publication in Astrophysics and Space Scienc

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The interacting subsystems theory of active galactic nuclei -- I. The broad-absorption-line QSO theory

Cited by 17 publications

References 40 publications

High-ion absorption in seven GRB host galaxies at z = 2–4

High-ion absorption in seven GRB host galaxies at z = 2–4

Absorption systems in the spectrum of GRB 021004

Matter Outflows from AGN: A Unifying Model

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