Ionization Driven Fragmentation of FeLoBAL Quasars

Ionization Driven Fragmentation of Gas Outflows Responsible for FeLoBALs in Quasars

Abstract

We show that time variations in the UV ionizing continuum of quasars, on scales of 1 year, affect the dynamic structure of the plasmas responsible for low ionization broad absorption lines. Variations of the ionizing continuum produce non-equilibrium photoionization conditions over a significant fraction of the absorbing clouds and supersonically moving ionization fronts. When the flux drops the contraction of the ionized region drives a supersonic cooling front towards the radiation source and a rarefaction wave in the opposite direction. The pressure imbalance is compensated by an increased speed of the cool gas relative to the front. When the flux recovers the cool gas is re-ionized and re-heated by a supersonic ionization front traveling away from the radiation source and a forward shock is created. The reheated clouds equilibrate to a temperature of  K and are observed to have different radial velocities than the main cloud. Such fragmentation seems consistent with the multicomponent structure of troughs seen in some objects. The velocity differences measured among various components in the quasars QSO 2359–1241 and SDSS J0318–0600 can be reproduced by our model if strong magnetic fields (10 mG) are present within the clouds.

1 Introduction

Gas outflows a potential source of feedback that regulates the evolution of the central black hole, the host galaxy, and the intergalactic medium (e.g. Elvis 2006). In the rest-frame UV spectra of 10 – 20% of all quasars (Knigge et al., 2008; Foltz et al., 1987), outflows are manifested in blueshifted Broad Absorption Lines (BAL). The most common of these are associated with resonance lines of medium ionization species, such as C iv, N v, O vi, Si iv, and H i and can reach velocities as high as 50,000 km (Weymann, 1995; Turnshek, 1995). Unfortunately, their saturated nature limits their utility in determining the physical characteristics of the outflow. A subset of BAL quasars, known as LoBALs, also show complexes of narrower (on the order of  km s) absorption features from low ionization species such as Mg ii, Al ii, and Si ii. Among these, objects that include troughs of metastable Fe ii or Fe iii are specifically called FeLoBALs. These are useful because the column densities of metastable levels offer valuable diagnostics of the outflow (Gabel et al. 2006; Arav et al. 2005; and references therein). These studies place the gas responsible for the FeLoBAL at distances between 1 kpc (Korista et al., 2008; Moe et al., 2009) and up to 10 kpc (Dunn et al., 2010).

We studied the various kinematic components in the FeLoBAL troughs of two quasars, QSO 2359–1241 and SDSS J0318–0600, 0.868 and 1.967 respectively (Bautista et al., 2010). It was found that among the various kinematic components the highest column density component of each system also had the highest particle density, while all other components have densities of about one quarter of that of the main component. Moreover, all the components seem to be located at the same distance from the central source, suggesting that they are all related to each other. This is also consistent with the finding of Voit et al. (1993) that BALs and LoBALs could be explained simultaneously by ablation of either a single large cloud or many scattered clouds.

Another characteristic of FeLoBALs is that, within the sample of known objects, they are borderline density-bounded. FeLoBAL quasars are seen in absorption from species that arise from the ionization front (IF) of the cloud (e.g. Si ii and Fe ii) while atoms from a neutral cold region, e.g. C i or Fe i, are not seen. This seems to point out some relationship between the ionization front and the nature of the clouds. The location of the IF of a cloud of a given density depends on the flux of hydrogen ionizing photons, particularly in the 1 to 4 Ryd energy range, from the radiation source. However, quasar continua are known to vary in the optical and UV within time scales of the order of one year (Kaspi et al., 2000). Hence, it is important to understand the effect of the varying radiation field on the structure of the FeLoBAL.

In this letter we show that when the flux that ionizes a FeLoBAL cloud drops the depth of the ionized region often shrinks at supersonic speeds followed by a cooling front, as explained in Sections 2 and 3. In section 4 we show that the supersonic cooling front creates a rarefaction wave, traveling in the opposite direction to the front, which results in fragmentation of the cloud. Under some conditions, such a fragmentation can explain the observed structure of FeLoBALs.

2 Magnitude scales and the effect of flux variations on FeLoBALs

Let us start with the simple picture illustrated in Fig. 1. Here, is the depth of the neutral region of the cloud and it is measured from the far end of the cloud towards the central source. For a given luminosity of the source and a cloud of constant particle density moving in a medium of negligible density one can draw an imaginary radius within which the cloud is fully ionized. This is

(1)

where is rate of hydrogen ionizing photons from the central source, is the recombination rate coefficient, and is the depth of the cloud. For a cloud located beyond the ionized depth () is related to the physical distance () as . Thus, FeLoBAL outflows that result from the formation of an IF, but without an extended neutral region, must be located right at . Then, a drop in the ionization flux, i.e. , will create a region of depth of either neutral or recombining plasma. Here, , where is total column density of the cloud and has a typical value of  cm. In deriving this equation we assumed that and . In QSO 2359–1241 and SDSS J0318–0600 are  cm and  cm and the sizes of the absorbers are  cm (i.e. 0.01 to 0.1 light-years). The change in the ionization of the gas is not instantaneous, but delayed by the recombination time scale of the plasma , with  scm at  K. Then,  yrs in QSO 2359–1241 and 100 yrs in SDSS J0318–0600. For example, in the case that is abruptly shut off, the size of the ionized region is

(2)

where is the time measured from the moment that the flux is turned off. Thus, the depth of the ionized region shrinks with a speed

(3)

Thus, from the derivation of and above  km s, which is much faster than the speed of sound in the plasma.

The width of quasi-static IFs is of the order of the mean free path for ionizing radiation, i.e. , where  cm is the photoionization cross section. Thus, the IF’s in QSO  2359–1241 and SDSS J0318–0600 are on the order of  cm, which are much smaller than the distance on which the IF retrats for flux variations on  year time scale. Still, these continuum variations much shorter than the recombination time will broaden the IF creating an extended recombining region. But, as the IF departs from ionization equilibrium it also departs from thermal equilibrium. In a static IF the temperature drops to a much lower value for a given value of the optical depth to heating photons. The optical depth is

(4)

with the neutral hydrogen density. Let us assume, for instance, a static IF of the form . As the ionized region shrinks the characteristic depth of the front increases to . At an early time after an instantaneous retreat of the IF . Thus, for an IF brodening by a factor it will take a time for the cooling front to start moving with the retreating IF. Then, if the value of for which the temperature drops remains constant the depth within the IF at which this happens, , will be reduced with respect to . For example, if the change in temperature occurred at in the static IF, for , for , and for . In the region of new lower equilibrium temperature cooling of the plasma proceeds much faster than recombination, because the cooling time scale is only  years (Spitzer, 1998). In conclusion, the drop in temperature closely follows the supersonic shrinking of the ionized region despite the broadening IF. Note that a drop in temperature makes recombination speed up, because increases as as the electron temperature decreases.

What happens when the flux increases again? As the ionizing flux rises the neutral fragment of the cloud will be re-ionized. Thus, an IF will travel through the neutral fragment, in the direction away from the ionizing source. This process is governed by the equation

(5)

The speed of the IF in this case is proportional by the change in radiative flux and can be highly supersonic, in which case it will send shocks ahead of the IF and rarefaction waves in the opposite direction.

In conclusion, time variations of the ionizing flux are expected to have two kinds of effects: (1) In the region neighboring the IF the ionization varies with time and departure from photoionization equilibrium could occur. This effect is out of the scope of this paper, but will be the subject of future investigation. (2) The varying ionizing flux will create supersonic cooling and heating fronts traveling through the ionized fraction of the cloud and the neutral region. These will be accompanied by rarefaction waves and shocks. This process is investigated in Section 4 of this letter, but first we will derive a more accurate description of the dynamics of the IF.

Figure 1: Illustration of a photoionized cloud of depth traveling away from the light source. The upper cloud is right at and the whole depth is ionized. In the lower cloud only a depth is ionized due to either a larger physical distance or a drop in .

3 Dynamics of ionization fronts within outflowing clouds

The IF within a cloud is defined as the region where the ionization drops to near zero. Thus, we solve for in the time dependent photoionization equation

(6)

Where is time, is the velocity of the gas, and and are the ionization and recombination rates per volume,

(7)
(8)

where is the optical depth within the cloud up to the depth .

Integrating Eqn. 3 in the co-moving frame of the IF () over the ionized volume , with the covering solid angle, one finds a differential equation for

(9)

For gas clouds much smaller than the distance to the ionizing source, i.e. , one can assume constant density during a crossing time of the cloud (). Then,

(10)

To understand this solution it is useful to check a couple of cases:

1) varying as a step function. Let us assume that at the absorber just reached when the continuum flux was . Thus, the cloud is fully ionized and a drop in will produce an IF. If the absorber were closer than it could remain fully ionized even when is reduced. If the flux drops to at for one gets

(11)

and

(12)

which is consistent with the result of equation (4) and yields supersonic for flux variations of or greater, i.e. .

Figure 2: Flux, , and for a sample of PG quasars observed by Kaspi et al. (2000). The results are for PG0844 (left panels), PG1226 (middle panels), and PG1411 (right panels). The calculations assume  yrs and  cm. The horizontal dotted lines in the vs. plots delimit the approximate range for subsonic motion.

2) from observed quasar continua. Here we compute the ionization of the cloud vs. time for selected quasar continua observed by Kaspi et al. (2000) using Eqn.(10). Fig. 2 shows the observer flux, the IF location with respect to the total depth of the cloud and for three quasars. These objects are chosen out of a sample of 17 quasars observed by Kaspi et al. because these illustrate the types of dynamical behaviors of the IF. Because the calculations are done for illustrative purposes only we disregard the uncertainties on the measured fluxes. Notice, for example, that in PG0844 the ratio is generally decreasing with time because the average ionizing continuum is lower than at the initial time of observation. This overall behavior is somewhat arbitrary as it depends on the initial observation. What is more meaningful, though, is the instantaneous velocity of the IF front, computed as , and this is seen to reach highly supersonic values. This is because the flux levels in PG0844, PG1226, and PG1411 vary by 40%, 50%, and 30% with respect to the value at in less than a year. Clearly, this determination of velocities is sensitive to the observational errors as well as the sampling of the quasar luminosity. Hence, we make no definitive claims on specific objects. However, the prediction that highly supersonic fronts are expected is supported in every object of the available sample.

4 Supersonic ionization fronts and cooling fronts

The supersonic IF is accompanied by a cooling front that leaves a pressure step behind. This creates a rearward-facing, i.e. in the opposite direction to the IF, rarefaction wave and a forward-facing shock (Strachan and Ahlborn, 1975; Ahlborn and Strachan, 1973). Under homogeneous conditions and for an infinite flow stream these waves and shocks will form periodically (Schnerr & Adam, 1997). As discussed before, the fragments once created become re-ionized and re-heated when the flux recovers. Then one can study the jump conditions between the main cloud and the fragments assuming constant temperature.

In one dimension the jump conditions across the rarefaction wave are

(13)
(14)
(15)

where is the mass density of the gas, is the bulk velocity of the gas in the co-moving frame of the wave (), is the thermal pressure, and is the strength of the magnetic field. Because the jump is essentially isothermal we adopt , and from Eqns. (13) - (15) one gets

(16)

where is the Alfven velocity. Thus, the difference of velocities between the fragments and the main cloud is

(17)

where we have used typical conditions and  km s. This result shows that rarefaction waves, originated by supersonic IF, yield lower density fragments that detach from the main cloud with relative velocities of tens of km s in absence of magnetic fields and much larger velocities when these are present.

There is evidence suggesting the presence of magnetic fields in BALs. Large trough widths, of the order of 100 km/s, are observed in FeLoBALS, with the largest widths being generally associated with the main absorber (see Table 1 of Bautista et al. 2010). The widths are much greater than expected from thermal broadening and seem to indicate supersonic turbulent velocities which could only be sustained by equally fast Alfven waves. The alternative scenario that observed trough widths could be mostly due to bulk velocity gradients along the line of sight is inconsistent with the fact that clouds have been able to travel  kpc away from the AGN without diffusing into the interstellar medium. Moreover, it is difficult to understand how bulk velocity gradients could yield similar trough profiles for ions with different ionization stages (but see Arav et al. 1999).

Strong magnetic fields in BAL clouds have been proposed in the past. de Kool and Begelman (1995) pointed out that magnetic pressures in BAL clouds must exceed thermal and radiative pressures to confine the clouds when accelerated up to thousands of km s. Their models for acceleration of BAL clouds yield magnetic field strengths of the order of 10 mG. Further, Furlanetto and Loeb (2001) argue that BAL quasar outflows could carry a large fraction of the magnetic energy of the intergalactic medium in clusters of galaxies. The source of such magnetic fields could be either from the accretion disc of the AGN (de Kool and Begelman, 1995), or from dynamo-like effects in the plasmas such as in the solar winds and supernova remnants (Giacalone and Jokipii, 2007; Kim and Balsara, 2006; Balsara and Kim, 2005).

We find that magnetic fields of the order of 10 mG, i.e. Alfven velocities of a few hundred km s, would explain the observed velocity separations between the main and the minor components as observed in QSO 2359–1241 and SDSS J0318–0600 (see Bautista et al. 2010).

Another interesting aspect of Eqn. (17) is that it predicts fragments that are faster than the main cloud as well as fragments that are slower than the main cloud, as seen in FeLoBALs. For example, since if  km s and  km s, then  km s and  km s. By contrast, if  km s then  km s and  km s. The faster clouds, in the rest frame of the quasar, are expected to outrun the main cloud and remain undisturbed by it. The survival of the slower clouds depends on the geometry of the problem. In one dimensional geometry the slow clouds would be swept up by the main cloud. In two and three dimensions it is possible that magnetic fields produce surface tension in the clouds capable of withstanding the fluid bulk pressure. The deceleration of the flow along the axis of travel of the main cloud and its fragments yields a bow shock, where the supersonic gas of the main cloud flows smoothly around the small fragment (see Shu 1992).

5 Discussion and Conclusions

We studied the effects of quasar time variable UV flux on FeLoBAL clouds. In these systems absorption from Si ii and Fe ii comes from a region just before an IF. This IF is formed within the absorbing cloud when the cloud crosses a distance from the radiation source. At this distance, when the radiation flux drops the ionized region of the cloud will retreat at supersonic speeds. A cooling front will follow the ionized region and the IF will also retreat and broaden. This creates a pressure imbalance across the IF on time scales much shorter than the sound crossing time. Thus, the cooling front yields a rarefaction wave that travels into the low temperature region. To conserve momentum across the cloud the large pressure imbalance is compensated by an increased speed of the cold gas relative to the front. Now, when the flux recovers the neutral rarefied region is re-ionized and re-heated by an IF moving away from the ionizing source. This IF can be highly supersonic, driving a shock ahead of it and a rarefaction wave in the opposite direction. The shocked gas forms new clouds and stabilize at a temperature of  K, like the main cloud. These clouds are detached in velocity space from the main cloud and there are rarefaction waves moving between the clouds.

There are two fundamental parameters in determining the speed of the retreating IF. One is the ratio of the depth of the cloud to the recombination rate, , which in turn is proportional to the column density of the cloud, . Thus, high column density clouds can have faster IFs. The other parameter is the ratio of the variability time scale of the ionizing source to the recombination time. Flux variations on scales of  year are enough for significant effects in FeLoBALs with particle densities of  cm, while variability on shorter time scales would affect higher density clouds. When the flux drops, broadening of the IF slows the cooling front down such that marginally supersonic IF may not lead to shocks and waves, but faster IFs will.

The thermal pressure imbalance across the IFs alone yields velocities to the fragments of the order of 20 km s with respect to the main cloud. Much higher velocities can be attained if sizable magnetic pressures are considered. Moreover, in two objects for which complete measurements exists, QSO 2359–1241 and SDSS J0318–0600, the observed separation between kinematic components is well reproduced by magnetic field strengths of the order of  mG.

Our model predicts that the detached fragments can be either faster or slower than the main cloud, as observed in FeLoBAL spectra. Survival of the slower fragments depends on the geometry of the problem. We propose that the slower fragments may permeate the main cloud if they are clumpy with a small filling factor and/or if the magnetic surface tension of the clouds is large enough to make the clouds flow around each other.

The physical effects presented here may not be exclusive to FeLoBALs, but could have implications in a variety of galactic and extragalactic phenomena. For example, in cataclysmic variables, variable stars with circumstellar envelopes such as Carinae, and in the narrow line regions of AGN.

We like to thank Nahum Arav and Kirk Korista for fruitful discussions. We also thank the anonymous referee for important suggestions.

References

  1. Ahlborn, B. and Strachan, J.D. 1973, Can. J. Phys. 51, 1416
  2. Arav, N., Kaastra, J., Kriss, G.A., Korista, K.T., Gabel, J., Proga, D. 2005, ApJ 620, 665
  3. Arav, N., Korista, K.T., de Kool, M., Junkkarinen, V.T., Begelman, M.C. 1999, ApJ 516, 27
  4. Arav, N., Li, Zhi-Yun, Begelman, M.C. 1994, ApJ 432, 62
  5. Arav, N., Moe, M., Costantini, E., Korista, K.T., Benn, C., Ellison, S. 2008, ApJ 681, 954
  6. Balsara, D.S. and Kim, J. 2005, ApJ 634, 390
  7. Bautista, M.A., Dunn, J.P., Arav, N., Korista, K., Moe, M., Benn, C. 2010, ApJ 713, 25
  8. Bautista, M.A. & Pradhan, A.K. 1998, ApJ 492, 650
  9. Blum, R.D., Pradhan, A.K., 1992, ApJS, 80, 425
  10. Brotherton, M.S., Arav, N., Becker, R.H., Tran, H.D., Gregg, M.D., White, R.L., Laurent-Muehleisen, S.A. & Hack, W. 2001, ApJ, 546, 134
  11. de Kool, M. and Begelman, M.C. 1995, ApJ 455, 448
  12. Dufton,P.L., Kingston,A.E., 1991, MNRAS, 248, 827
  13. Dunn, J., Bautista, M.A., Arav, N., Moe, M., Korista, K.T., Constantini, E. Benn, C., Ellison, S., Edmonds, D. 2010, ApJ 709, 611
  14. Dunn, J., Crenshaw, D.M., Kraemer, S.B., Trippe, M.L. 2008 AJ 136, 136
  15. Ferland, G.J., Korista, K.T., Verner, D.A., Ferguson, J.W., Kingdon, J.B., Verner, E.M. 1998, PASP 110, 761
  16. Foltz, C.B., Weymann, R.J., Morris, S.L., Turnshek, D.A. 1987, ApJ 347, 450
  17. Furlaneto, S.R. and Loeb, A. 2001, ApJ 556, 619
  18. Gabel, J. R., Arav, N., Kim, T. 2006, ApJ, 646, 742
  19. Ganguly, R. & Brotherton, M. S. 2008, ApJ, 672, 102
  20. Giacalone, J. and Jokipii, J.R. 2007, ApJ 663, L41
  21. Hamann, F., Kaplan, K.F., Hidalgo, P.R., Prochaska, J.X., Herbert-Fort, S. 2008, MNRAS 391, L39
  22. Hamann, F., Kaplan, K.F., Hidalgo, P.R., Prochaska, J.X., Herbert-Fort, S. 2008, MNRAS 391, L39
  23. Kaspi, S., Smith, P.S., Netzer, H., Maoz, D., Jannuzi, B.T., Giveon, U. 2000, ApJ 533, 631
  24. Kim, J. and Balsara, D.S. 2006, Astron. Nachr. 327, 433
  25. Knigge, C., Scarini, S., Goad, M.R., Cottis, C.E. 2008, MNRAS 386, 1426
  26. Korista, K.T., Bautista, M.A., Arav, N., Moe, M., Constantini, E., Benn, C. 2008, ApJ 688, 108
  27. Moe, M., Arav, N., Bautista, M.A., Korista, K.T. 2009 ApJ 706, 525
  28. Nussbaumer H., 1977, A&A 58, 291
  29. Schnerr, G.H. and Adam, S. 1997, J. of Thermal Scisnce, 6, 171
  30. Shu, F.H. 1992, ”The Physics of Astrophysics. Volume II: Gas Dynamics”, University Science Books, Mill Valley CA, USA
  31. Spitzer, L. in Physical Processes in the Interstellar Medium, Ed. Wiley-Interscience Publication, New York, pp. 139
  32. Strachan, J.D. and Ahlborn, B. 1975, Aust. J. Phys. 28, 395
  33. Trump, J. R. et al. 2006, ApJS, 165, 1
  34. Turnshek, D.A. 1995, in QSO Absorption Lines, ed. G. Meylan (Berlin: Springer), 223
  35. Voit, G.M. Weymann, R.J., Korista, K.T. 1993, ApJ 413, 95
  36. Weymann, R.J. 1995, in QSO Absorption Lines, ed. G. Meylan (Berlin: Springer), 213
  37. Wiese W.L., Fuhr J.R., 1995, NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
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