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Cited by 17 publications
(19 citation statements)
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References 48 publications
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“…Hamann et al (2013) suggests that mini-BAL absorbers consist of a number of small gas clouds (d cloud ≤ 10 −3 -10 −4 pc) with very large gas density (n e ≥ 10 6 -10 7 cm −3 ) at the absorber's distance of r ∼ 2 pc to avoid over-ionization. A similar picture is also suggested for BAL quasars (Joshi et al 2014). Furthermore, recent radiation-MHD simulations by Takeuchi et al (2013) reproduce variable clumpy structures with typical sizes of ∼ 20 r g in warm absorbers, corresponding to ∼ 5×10 −4 pc assuming the black-hole mass of SDSS J1029+2623, M BH ∼ 10 8.72 M ⊙ .…”
Section: Detectability Of Sightline Differencesupporting
confidence: 74%
“…Hamann et al (2013) suggests that mini-BAL absorbers consist of a number of small gas clouds (d cloud ≤ 10 −3 -10 −4 pc) with very large gas density (n e ≥ 10 6 -10 7 cm −3 ) at the absorber's distance of r ∼ 2 pc to avoid over-ionization. A similar picture is also suggested for BAL quasars (Joshi et al 2014). Furthermore, recent radiation-MHD simulations by Takeuchi et al (2013) reproduce variable clumpy structures with typical sizes of ∼ 20 r g in warm absorbers, corresponding to ∼ 5×10 −4 pc assuming the black-hole mass of SDSS J1029+2623, M BH ∼ 10 8.72 M ⊙ .…”
Section: Detectability Of Sightline Differencesupporting
confidence: 74%
“…Significant variation of BALs, including a complete disappearance, with a time scale of 1-10 year in the quasar restframe have been reported in the previous studies (e.g., Hall et al, 2011;Zhang et al, 2011Zhang et al, , 2015Filiz Ak et al, 2012Vivek et al, 2012Vivek et al, , 2014Joshi et al, 2014). The significant variation can be explained by a variation of either the ionizing power (e.g., Trevese et al, 2013) or the covering factor due to a cloud transiting the line-of-sight (e.g., Hall et al, 2011).…”
Section: Non-variation Of the New Ofelobal Quasarmentioning
confidence: 61%
“…Using the multiepoch observations they have found a synchronous kinematic shift of C iv, Si iv, and N v absorption features, while preserving the absorption profile, with a varying deceleration rate which raises from −0.1 ± 0.03 cm s −2 to −0.25 ± 0.05 cm s −2 in the later interval. In addition, Joshi et al (2014) have detected relatively larger deceleration rate of −0.7 ± 0.1 cm s −2 and −2.0 ± 0.1 cm s −2 of C iv BAL in two X-ray bright BAL quasars over restframe time-spans of 3.11 and 2.34 years. Recently, Grier et al (2016) have performed the first systematic search for BAL acceleration using three epoch SDSS spectra of 140 BAL quasars over timescales of 2.5−5.5 years and found only 3 cases, two acceleration and one deceleration, of monolithic velocity shift showing an overall lack of widespread BAL acceleration.…”
Section: Discussionmentioning
confidence: 87%
“…In our BAL variability studies of X-ray bright BALQ-SOs till now we have found significant profile shift in three cases. Joshi et al (2014) reported two cases of deceleration-like signatures. Unlike in the present case the deceleration is also accompanied by profile shape variation in other two cases.…”
Section: Discussionmentioning
confidence: 99%
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