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The current shee she. the magnetopause and the peripatopause. constitute discontinuities for the magnetic pressure. DpDd/Nz. the eas pressure. pi. the temperature. Ti. and the density. pi. | The current sheets, i.e. the magnetopause and the peripatopause, constitute discontinuities for the magnetic pressure, $B^2_{\rm b}/8\pi$, the gas pressure, $p_{\rm b}$, the temperature, $T_{\rm b}$, and the density, $\rho_{\rm b}$. |
But uote. that when crossing the current sheets horizontally. the total pressure (gas plus magnetic) is coustant. | But note, that when crossing the current sheets horizontally, the total pressure (gas plus magnetic) is constant. |
An eusemible of inagnetie flux tubes is assuned to participate in inuterclauuge convection. | An ensemble of magnetic flux tubes is assumed to participate in interchange convection. |
As a first step we restrict the study to simulations of the evolution of a single flux tube. | As a first step we restrict the study to simulations of the evolution of a single flux tube. |
Iu this contribution. we prescut the results obtained for one specific fiux tube aud concentrate mainly ou its plotospheric behavior. | In this contribution, we present the results obtained for one specific flux tube and concentrate mainly on its photospheric behavior. |
The results preseuted iu this section have been obtained for the tube with a maguetic flux o=2-10/9 Mx. | The results presented in this section have been obtained for the tube with a magnetic flux $\phi = 2\cdot 10^{16}$ Mx. |
That corresponds to a diameter of d=2+y/o/DB=50 ku. for a 1naegnetic field streugth equal to 1000. C. Initially. the tube lies along the magnetopause. | That corresponds to a diameter of $d = 2\cdot \sqrt{\phi/B\pi}= 50$ km, for a magnetic field strength equal to 1000 G. Initially, the tube lies along the magnetopause. |
Ivdrostatie equilibriuna along the tube is satisfied since the distribution of the density and temperature is ideutical with the peuunbral stratification: Maeuetostatic equilibrium. 1.6. the cancellation of the second and third term on the ROS of ((20)). Is an intrinsic property of the tripartite model. and can be realized nuuercallv with an accuracy which is sufficient. but limited by the imerpolation procedures. | Hydrostatic equilibrium along the tube is satisfied since the distribution of the density and temperature is identical with the penumbral stratification: Magnetostatic equilibrium, i.e., the cancellation of the second and third term on the RHS of \ref{dvsenk}) ), is an intrinsic property of the tripartite model, and can be realized numerically with an accuracy which is sufficient, but limited by the interpolation procedures. |
The magnetic field strength is eiven by the total pressure equilibrium across the maguetopaise. The τοςοἱπρο extends down to a depth of «=15 Nn at a radial distance of «=L8 Maii. | The magnetic field strength is given by the total pressure equilibrium across the magnetopause, The model-tube extends down to a depth of $z= -15$ Mm at a radial distance of $x=4.8$ Mm. |
The upper cud is placed at a radial distance of μι=21 Alin and at a | The upper end is placed at a radial distance of $x=24$ Mm and at a |
The XRT data reduction was performed using the standard daa pipeline package v. 0.12.6). in order to produce screcued eveut files. | The XRT data reduction was performed using the standard data pipeline package v. 0.12.6), in order to produce screened event files. |
All data were extracted only iu the photon counting (PC) mode (ITill et al. | All data were extracted only in the photon counting (PC) mode (Hill et al. |
2001). adopting the standard erade filterine (0.12 for PC) according to the NRT nomenclature. aud usine au extraction radius of 21". | 2004), adopting the standard grade filtering (0–12 for PC) according to the XRT nomenclature, and using an extraction radius of $''$. |
Within the observation we analysed. with the tool v. Lid. the 0.310 keV nuage to search for sources detected (at a confidence level 236) both at the optical position of star CCS 5926 aud inside theROSAT error circle. | Within the observation we analysed, with the tool v. 4.4.1, the 0.3–10 keV image to search for sources detected (at a confidence level $>$ $\sigma$ ) both at the optical position of star CGCS 5926 and inside the error circle. |
Iun parallel witji the Nvay poiuting. he UltraViolet-Optical Telescope (UVOT: Roming et a. | In parallel with the X–ray pointing, the UltraViolet-Optical Telescope (UVOT; Roming et al. |
2005) onboard as well. observed COS 5926 in tιο CVA2 baud (A = 2216As: full width at half masiniu: d98 ÀJ) fora total of 1361 s starting at 08:37:12 UT of 6 January 2010. | 2005) onboard as well, observed CGCS 5926 in the $UVM2$ band $\lambda$ = 2246; full width at half maximum: 498 ) for a total of 4364 s starting at 08:37:42 UT of 6 January 2010. |
Count rates were measured through aCrire photometry usingM] it apertures and were calibrated 1sug the UVOT photometric svstem described by Poole e al. ( | Count rates were measured through aperture photometry using $''$ apertures and were calibrated using the UVOT photometric system described by Poole et al. ( |
2008). | 2008). |
The optical spectrum of COCS 5926 (Figs. | The optical spectrum of CGCS 5926 (Figs. |
2 aud 3) clearly shows the typical features of a carbon star (Yamashita 1967: Cohen et al. | 2 and 3) clearly shows the typical features of a carbon star (Yamashita 1967; Cohen et al. |
1996): it is unndstakablv dominated by the Cy Swan bands at L737. 5165 and 5635 in the blue. and by CN bands rechwards. | 1996): it is unmistakably dominated by the $_2$ Swan bands at 4737, 5165 and 5635 in the blue, and by CN bands redwards. |
We also find. among the main spectral features. the Na doublet at 5890 and two atomic line bleuds of metal iutersvste lines of FeIL. Tit Cri. Da1. Cad. Mui. Co and Ni located at 6352 and 697 (see e.g. Turushek et al. | We also find, among the main spectral features, the Na doublet at 5890 and two atomic line blends of metal intersystem lines of Fe, Ti, Cr, Ba, Ca, Mn, Co and Ni located at 6352 and 6497 (see e.g. Turnshek et al. |
1985). | 1985). |
A telluric absorption feature is preseut at 7605A. | A telluric absorption feature is present at 7605. |
No enission features typical ofX.rav binaries. such as Balmer and We lines are present. | No emission features typical of X–ray binaries, such as Balmer and He lines are present. |
Iu particular. no IL, or IL; lines are readily detected either in emissiou or in absorption. | In particular, no $_\alpha$ or $_\beta$ lines are readily detected either in emission or in absorption. |
Moreover. the spectriuui shown in Fig. | Moreover, the spectrum shown in Fig. |
3 aud coveriis he blue raice of COCS 5926 clearly indicates that there Is no evident excess in the ( baud. as no signal is detected rol this oject bluewiud of ~ 1200À. | 3 and covering the blue range of CGCS 5926 clearly indicates that there is no evident excess in the $U$ band, as no signal is detected from this object blueward of $\sim$ 4200. |
. This cofirs f1e ack of sigwl detection in the blue part of t16 Ásiago spectra acquired earlier. which is however not surprisi18o eivon the red giant nature of the star couple with t1ο aree optical absorption we infer toward it (see below). | This confirms the lack of signal detection in the blue part of the Asiago spectra acquired earlier, which is however not surprising given the red giant nature of the star coupled with the large optical absorption we infer toward it (see below). |
Usiug he two-dimensional CGn.n) ¢lagnostics of Yinashita (1967) and the quantitative classification scheme derived by Cohen (1979). we can better classify the spectral type of CGCS 5926. | Using the two-dimensional $m$ $n$ ) diagnostics of Yamashita (1967) and the quantitative classification scheme derived by Cohen (1979), we can better classify the spectral type of CGCS 5926. |
Conceruing the a) parameter. which is associated with the temperature index 7. we fiud from our optical spectirmim of ιοο 5926 shown in Fig. | Concerning the $m$ parameter, which is associated with the temperature index $T$, we find from our optical spectrum of CGCS 5926 shown in Fig. |
2 that £ = 0.15z:0.03: this. frou: Table 2 of Cohen (1979) nuplies that a = 6. which corresponds to an effective. blackbody temperature Tig& 2500 I& (Cohen 1979: Berecat et al. | 2 that $T$ = $\pm$ 0.03: this, from Table 2 of Cohen (1979) implies that $m$ = 6, which corresponds to an effective blackbody temperature $T_{\rm eff}
\approx$ 2500 K (Cohen 1979; Bergeat et al. |
2001). | 2001). |
Likewise. the carbon iudices C1. C2 aud C3 are 0.51250.04. 0.582EO.0 EL and 0.90£0.06. respectively. shich allow us to infer that ο = 2 (see Table 3 of Cohen 1979). | Likewise, the carbon indices $C1$, $C2$ and $C3$ are $\pm$ 0.04, $\pm$ 0.04 and $\pm$ 0.06, respectively, which allow us to infer that $n$ = 2 (see Table 3 of Cohen 1979). |
Therefore. we are able to classify the spectitun of COCS 5926 as C(6.2). | Therefore, we are able to classify the spectrum of CGCS 5926 as C(6,2). |
We note that the use of the diagnostic D of Cohen et al. ( | We note that the use of the diagnostic $D$ of Cohen et al. ( |
1996) instead of the temperature index T for the determination of he paraleter i ives us a somewhat lower vaue (around 5.5). uuplvine a slightly ligher temperature and thus an earlier spectral type. | 1996) instead of the temperature index $T$ for the determination of the parameter $m$ gives us a somewhat lower value (around 5.5), implying a slightly higher temperature and thus an earlier spectral type. |
The results of our photometry of COCS 5926 are reported in Table 1. | The results of our photometry of CGCS 5926 are reported in Table 1. |
These indicate that the source shows a variability of amplitude Am~ 0.3 1nag on timescales of tens of davs. | These indicate that the source shows a variability of amplitude $\Delta m \sim$ 0.3 mag on timescales of tens of days. |
Moreover. the VReo aud Re:Te: color iudices of COCS 5926 seem tfo eet stnaller as he V-baud magnitude decreases: that is. fie star gets quer with increasing brielituess. | Moreover, the $V-R_{\rm C}$ and $R_{\rm C}-I_{\rm C}$ color indices of CGCS 5926 seem to get smaller as the $V$ -band magnitude decreases; that is, the star gets bluer with increasing brightness. |
Therefore we carried out a periodicity search on the photometric data usine he Fourier code of Decmüng (1975). | Therefore we carried out a periodicity search on the photometric data using the Fourier code of Deeming (1975). |
À siele, strong xobabilitv peak was found at a period of 151 davs. | A single, strong probability peak was found at a period of 151 days. |
The ephemeris we obtained with this period. expressed iu Uchocentric Julian Days (IIJDs). provides t1e. following nues of mania in the V. baud: where Fis au integer απο: the errors are at Jo confidence level. | The ephemeris we obtained with this period, expressed in Heliocentric Julian Days (HJDs), provides the following times of maxima in the $V$ band: where $E$ is an integer number; the errors are at $\sigma$ confidence level. |
The V-baud aud the V.Ze: color light curves of COCS 5926 folded onto this ephemeris are Mese itedin Fig. | The $V$ -band and the $V-I_{\rm C}$ color light curves of CGCS 5926 folded onto this ephemeris are presented in Fig. |
LL | 4. |
Their shape. aud the fact that the star eots quer at nium and redder at nuininmuu optical xiehtuess. Sugeest that this variability traces the radial oilsaion of this carbon star (see e.g. Wallersteiu nap 1995). | Their shape, and the fact that the star gets bluer at maximum and redder at minimum optical brightness, suggest that this variability traces the radial pulsation of this carbon star (see e.g. Wallerstein Knapp 1998). |
Because of the relatively short time baseline coverea X our observations ( LOO davs. that is. a bit more tha- wo pulsation cevcles). we cannot 11id a 1nean light curve (i.c. one averaged over several aud well covered pulsatio- evcles) for the star. | Because of the relatively short time baseline covered by our observations $\sim$ 400 days, that is, a bit more than two pulsation cycles), we cannot build a mean light curve (i.e. one averaged over several and well covered pulsation cycles) for the star. |
Twis. the only feasible approach te estimate he above crrors on the oxxiod and the epoc[um was fo Hnupose that fje. lighteu« ds the simplest aud sootlest possible. wi ha shape similar to that of other objects o that variability class (1ji this case. a rise to nani faster than he decline to init). | Thus, the only feasible approach to estimate the above errors on the period and the epoch was to impose that the lightcurve is the simplest and smoothest possible, with a shape similar to that of other objects of that variability class (in this case, a rise to maximum faster than the decline to minimum). |
Besices. we stress tha these stars usually display a significant variability of the perio and epoch wit1 fiae around mca values (possibly due te) beating of multiple periodicities: see Wallerstein Ixuayp 1998 aud references therein). | Besides, we stress that these stars usually display a significant variability of the period and epoch with time around mean values (possibly due to beating of multiple periodicities; see Wallerstein Knapp 1998 and references therein). |
One can then estinate the distance to COCS 5926 in the folowing manner. | One can then estimate the distance to CGCS 5926 in the following manner. |
Assuming an average magnitude VelLsfortje source. its JAZ, magnitudes as reported in the 2MLASS catalog (see Section 1) and the intrinsic color indices Or carbon stars as reported iu Table 6 of Ducati ¢ al. ( | Assuming an average magnitude $V \sim$ 14.8 for the source, its $JHK_{\rm
s}$ magnitudes as reported in the 2MASS catalog (see Section 1) and the intrinsic color indices for carbon stars as reported in Table 6 of Ducati et al. ( |
2001). one gets an average optical reddening Ay~ 3.8 mag. which corresponds to a color excess E(B 1.23 mae considering the Galactic absorption law of Cardeli et al. ( | 2001), one gets an average optical reddening $A_V \sim$ 3.8 mag, which corresponds to a color excess $E(B-V) \sim$ 1.23 mag considering the Galactic absorption law of Cardelli et al. ( |
1989) aud a total-to-selective extinction | 1989) and a total-to-selective extinction |
eravitational component. which was used to scale. the o»wvonie component properties. (77).. | gravitational component, which was used to scale the baryonic component properties \citep{2007MNRAS.380.1369T,
2009ApJ...694..842M}. |
Lo this paper. we implement. radiation hvdrodynamies using the algorithm of ?. coupled to the gravity-hydrodynamies code (specifically v1.0.1). | In this paper, we implement radiation hydrodynamics using the algorithm of \citet{BMW04} coupled to the gravity-hydrodynamics code (specifically v.1.0.1). |
Phe hyvdrodynamical response of the eas to the boost in heating when radiative transfer is included: could: result. in. more rapid. photo-evaporation of he eas in small haloes. allowing reionization to occur more rapidly. as well as in observational signatures on the forest such as increased line broadening due to outllows rom the haloes and a decrease in the ratio of gas density o dark matter density. | The hydrodynamical response of the gas to the boost in heating when radiative transfer is included could result in more rapid photo-evaporation of the gas in small haloes, allowing reionization to occur more rapidly, as well as in observational signatures on the forest such as increased line broadening due to outflows from the haloes and a decrease in the ratio of gas density to dark matter density. |
An increase in the gas temperature will also alter. the ionization fractions of hydrogen ancl ielium at a given gas density. producing mocifications to the column densities of the absorption features. the distribution "unction of pixel Uuxes. and the flux. power spectrum. all rasic statistics used to quantify the forest and the predictions of cosmological models for. its structure. | An increase in the gas temperature will also alter the ionization fractions of hydrogen and helium at a given gas density, producing modifications to the column densities of the absorption features, the distribution function of pixel fluxes, and the flux power spectrum, all basic statistics used to quantify the forest and the predictions of cosmological models for its structure. |
All results. are. for a Hat ACDAL universe with the cosmological parameters O,,=0.24. O,h?=0.022 and h=Haf/100kms+0.73. representing the total mass density. barvon density and Hubble constant. respectively. | All results are for a flat $\Lambda$ CDM universe with the cosmological parameters $\Omega_m=0.24$, $\Omega_bh^2=0.022$ and $h=H_0/100~\kms=0.73$, representing the total mass density, baryon density and Hubble constant, respectively. |
The power spectrum has spectral index à=0.95. ancl is normalized to my),1=0.14. | The power spectrum has spectral index $n=0.95$, and is normalized to $\sigma_{8h^{-1}}=0.74$. |
This paper is organized as follows. | This paper is organized as follows. |
Estimates for the expected IGM temperature boost following rreionization are cliscussed in. the next section. | Estimates for the expected IGM temperature boost following reionization are discussed in the next section. |
The simulations are described in Sec. | The simulations are described in Sec. |
3 and the results presented in Sec. | 3 and the results presented in Sec. |
4. | 4. |
The aand sspectral signatures of rreionization are presented in Sec. | The and spectral signatures of reionization are presented in Sec. |
5. | 5. |
A comparison with approximate simulation methods is provided in Sec. | A comparison with approximate simulation methods is provided in Sec. |
6. | 6. |
The principal conclusions are summarised in the final section. | The principal conclusions are summarised in the final section. |
AX gadiation field with its specific energy density locally approximated near the pphotoelectric edge by a.=πει) will. photoionize the aat the rate per iion where £j is the frequcney of the LLyman edge and the photoionization cross-section is approximated as σοσυν) | A radiation field with its specific energy density locally approximated near the photoelectric edge by $u_\nu=u_L(\nu/\nu_L)^{-\alpha}$ will photoionize the at the rate per ion where $\nu_L$ is the frequency of the Lyman edge and the photoionization cross-section is approximated as $\sigma\simeq\sigma_0(\nu/\nu_L)^{-3}$. |
The corresponcing heating rate per lion is The heating rate per ionization. normalized bv the ionization potential. is thena). | The corresponding heating rate per ion is The heating rate per ionization, normalized by the ionization potential, is then. |
The energy injected into the gas is thus sensitive to the shape of the local ionizing spectrum. | The energy injected into the gas is thus sensitive to the shape of the local ionizing spectrum. |
X hardened radiation field with a«0 can result in a [large amount of energy deposited per ionization. | A hardened radiation field with $\alpha<0$ can result in a large amount of energy deposited per ionization. |
The spectrum is expected to. harden within an ionization front because hard. photons are less likely to be absorbed than soft photons above the photocletric threshold [or a given optical depth at the. threshold. energy. | The spectrum is expected to harden within an ionization front because hard photons are less likely to be absorbed than soft photons above the photoeletric threshold for a given optical depth at the threshold energy. |
1n eeneral. for à column density IN the optical depth above the photoelectrie threshold of hvdrogen or singly ionized helium is TeC9TLfL) where rj=ayN. | In general, for a column density $N$ the optical depth above the photoelectric threshold of hydrogen or singly ionized helium is $\tau_\nu\simeq\tau_L(\nu/\nu_L)^{-3}$ where $\tau_L=\sigma_0N$. |
The photoionization rate per atom/ion mav be expressed in terms of the incident radiation density from the source i;=up(vier)"7 as where 5(a..c)=dic(i leis the incomplet.e ganinma function. | The photoionization rate per atom/ion may be expressed in terms of the incident radiation density from the source $u^S_\nu=u^S_L(\nu/\nu_L)^{-\alpha_S}$ as where $\gamma(a,x)=\int_0^x\,dt\,e^{-t}t^{a-1}$ is the incomplete gamma function. |
Similarly. theI heating rate per atom/ion is The resulting heating rate per ionization of wwill produce a temperature increment where 7; is the initial gas temperature μηCY(he forLeu. | Similarly, the heating rate per atom/ion is The resulting heating rate per ionization of will produce a temperature increment where $T_i$ is the initial gas temperature and $\epsilon_{\HeII}=G/(h\nu_L\Gamma)$ for. |
The increment: corresponds to. the complete PV)ionization of to aal fixed τι. as would occur in the presence of an intervening Lyman limit svstem. already in ionization equilibrium. bing oween the source and the region being photoionized if he Lyman limit svstem dominated the optical depth at the Lyman edge. | The increment corresponds to the complete ionization of to at fixed $\tau_L$, as would occur in the presence of an intervening Lyman limit system, already in ionization equilibrium, lying between the source and the region being photoionized if the Lyman limit system dominated the optical depth at the Lyman edge. |
The radiation field reaching the region being xhotoionized would be hardened. by the absorption within he intervening system. | The radiation field reaching the region being photoionized would be hardened by the absorption within the intervening system. |
The temperature increment is shown as a function of the optical depth τι at the LLyman edge for a range of source spectral indices in Fig. | The temperature increment is shown as a function of the optical depth $\tau_L$ at the Lyman edge for a range of source spectral indices in Fig. |
1 (upper set of curves). | \ref{fig:temperature} (upper set of curves). |
A helium mass fraction of Y=0.248 was adopted (?).. | A helium mass fraction of $Y=0.248$ was adopted \citep{2007ARNPS..57..463S}. |
X system with overcensity ορ) and comoving thickness L would have an optical depth at. the LLyman edge of The radiation hardening through overcense systems with p/iíp)~200 and comoving sizes of 0.050.25 kpe would produce temperature boosts in the "shadows? they cast in less dense. more quickly photoionizecl structures. of up to AY~40000 Ex. and even reaching 107 [x in the shadows of intervening svstems with rpηc 100. | A system with overdensity $\rho/\langle\rho\rangle$ and comoving thickness $L$ would have an optical depth at the Lyman edge of The radiation hardening through overdense systems with $\rho/\langle\rho\rangle\sim200$ and comoving sizes of $0.05-0.25$ kpc would produce temperature boosts in the “shadows” they cast in less dense, more quickly photoionized structures, of up to $\Delta
T\simeq40000$ K, and even reaching $10^5$ K in the shadows of intervening systems with $\tau_{L, {\rm HeII}}>100$ . |
aud NEUS). | and ). |
It is stil a puzzle that the liue dux appears to be constant iu spite of strong contijuu1 variation. and that the EW is auti-correlaed with the coutimmiun flux as im MC(CC-6-30-15 (Leeetal.2000) and NGC€C55[5 (Chiangetal.2000).. | It is still a puzzle that the line flux appears to be constant in spite of strong continuum variation, and that the EW is anti-correlated with the continuum flux as in MCG-6-30-15 \citep[]{lee00} and NGC5548 \citep[]{chiang99}. |
This was explained by the presence of a hot ionized skin oan accretio- cisk induced x thermal instability (Navakshin.KIazanas&Wallan2000) or the resonant trapping folOWC( by Auger desruction in au ionized disk wich suppresses t1e enission of the line 2001). | This was explained by the presence of a hot ionized skin of an accretion disk induced by thermal instability \citep[]{nkk00} or the resonant trapping followed by Auger destruction in an ionized disk which suppresses the emission of the line \citep[]{brf01}. |
. ITowvever. ionization plysics in the immer disk is uulikelv to explain the behavior oiro line variation. at least in AICC-6-30-15 since the hue profile suggests the existence of cold material withi a radius of SAL (Iwasawactal.1999:Zvcαἱ&Roézatska2OL). | However, ionization physics in the inner disk is unlikely to explain the behavior of line variation, at least in MCG-6-30-15 since the line profile suggests the existence of cold material within a radius of $5M$ \citep[]{iwa99,zr01}. |
The variation of the ine profile i1 AMCG-6-30-15 (and possibly also in δις55) may be explained by the out-flowing magnetic flares mode1 in which the bulk motion aud location of flares may vary Jog. as discussed by Twasawactal.(1999)]]. | The variation of the line profile in MCG-6-30-15 (and possibly also in NGC5548) may be explained by the out-flowing magnetic flares model in which the bulk motion and location of flares may vary [e.g. as discussed by \citet[]{iwa99}] ]. |
A subsequent question is: can the bulk motion aud location oanaenetic fares cousistcuthy explaii the patter- of the variation iu liue intensity and EW corresponding to siguificaut variatious in continuum fux? | A subsequent question is: can the bulk motion and location of magnetic flares consistently explain the pattern of the variation in line intensity and EW corresponding to significant variations in continuum flux? |
On occasioji the N-vay cussion ds dominated by a sinele (or a small uuuber of) huge flare(s) or ucielboring flares (e.g.Poutanen&Fabian1999): but typically the N-rav. cussion nav be a sun of a dozen or πο overappiug flares. | On occasion, the X-ray emission is dominated by a single (or a small number of) large flare(s) or neighboring flares \citep[e.g.][]{pf99}; but typically the X-ray emission may be a sum of a dozen or so overlapping flares. |
In the special case where the X-ray cussion iu au object at any elven tine is douinated by a single flare or neighboring flares iu the imrer region (015M ). a significaif ο ilhiinatiou ofthe accretion disk is produced. | In the special case where the X-ray emission in an object at any given time is dominated by a single flare or neighboring flares in the inner region $r\simlt 15M$ ), a significant non-axisymmetric illumination of the accretion disk is produced. |
If fares produce at different time have siuil iutriusic N-raw ΠΠ but love outward/imward with different bulk velocities. then the resultiuο liue fiX appears constaut while the observed couiuuuu fux niuCreocs rapid variability due to f1ο σας effect f) a observer with a inclination =30° (see Fig. 8)). | If flares produced at different time have similar intrinsic X-ray luminosity, but move outward/inward with different bulk velocities, then the resulting line flux appears constant while the observed continuum flux undergoes rapid variability due to the beaming effect to a observer with a inclination $\la 30\arcdeg$ (see Fig. \ref{fig:offaxisrew70}) ). |
It is obvious hat a constant line flux cau also lx5 obtained from a coutiuuous corona (or a large uuuber of overlappiug flares) with varviis milk velocity iii tli region (r215M. απλοίο illumination) by averaeiic the sviubols for the flares wit sale bulk veloci but different azimuthal angles iu Fie. 8.. | It is obvious that a constant line flux can also be obtained from a continuous corona (or a large number of overlapping flares) with varying bulk velocity in the region $r\simlt 15M$, axisymmetric illumination) by averaging the symbols for the flares with same bulk velocity but different azimuthal angles in Fig. \ref{fig:offaxisrew70}. |
Therefore. the model o out-flowing maceic flares qualitative explains the observational behavior of the lue im MCC-6-:0-10 (Leeetal.WO) aud δις955 (CHanectal.2000).. | Therefore, the model of out-flowing magnetic flares qualitatively explains the observational behavior of the line in MCG-6-30-15 \citep[]{lee00} and NGC5548 \citep[]{chiang99}. |
These two objects are both coustraied to have eclinatious of 30° youn fits of the line profile with a relativistic disk liic. | These two objects are both constrained to have inclinations of $30\arcdeg$ from fits of the line profile with a relativistic disk line. |
The line in \CO-6-30-15 shows «Lenatic variability: it Was narrow duriie a hieh-flux state and very broad during a ¢eep-minima flix. but th otal line flux seenis o be constant curing the loug oervatiou in 1991 (Iwasawaeal.1996): however. its blue part is shifted well below 6.1 keV during a short bright period iu the long observation i1 1997 1999). | The line in MCG-6-30-15 shows dramatic variability: it was narrow during a high-flux state and very broad during a deep-minimum flux, but the total line flux seems to be constant during the long observation in 1994 \citep[]{iwa96}; however, its blue part is shifted well below 6.4 keV during a short bright period in the long observation in 1997 \citep[]{iwa99}. |
. Iuterestingly. the line profile has a huge red tail iu the deep-uiniuin111 specruni. ali the ine profile is wihout the 6.1 keV componen during the bright perio. | Interestingly, the line profile has a huge red tail in the deep-minimum spectrum, and the line profile is without the 6.4 keV component during the bright period. |
These observat1ος sugeesto that the N-ray source is very close to the ceutral black hole aud probably witun radius of GAL. | These observations suggest that the X-ray source is very close to the central black hole and probably within radius of $6M$. |
1: most of t ο ds indeed cnutted from the immer region with a typical radius of GAL in AICCC-6-30-15. the va flucnation o the lk velocity of fares in the rauge O.1 to 0. (sce Fig. 8)). | If most of the X-ray is indeed emitted from the inner region with a typical radius of $6M$ in MCG-6-30-15, then a fluctuation of the bulk velocity of flares in the range $-0.1$ to $0.1$ (see Fig. \ref{fig:offaxisrew70}) ), |
together with the non-axisviinetric iluiination due to the difference in the location of flares (this non-axisvninieric illumination should be averaged iu a long time interval) can account for the οoervatioual behavior of he line (Leoetal.20nn. | together with the non-axisymmetric illumination due to the difference in the location of flares (this non-axisymmetric illumination should be averaged in a long time interval) can account for the observational behavior of the line \citep[]{lee00}. |
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