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1991. their fig. | 1991, their fig. |
11). | 11). |
The clleets of the age-extinction clegeneracy are ramatic for this sample. however. | The effects of the age-extinction degeneracy are dramatic for this sample, however. |
On average. we find ju if we had not assumed a fixecl extinction. value. rw resulting ages would have. been smaller. (although rere remains significant scatter about the dashed. line of quality). | On average, we find that if we had not assumed a fixed extinction value, the resulting ages would have been smaller (although there remains significant scatter about the dashed line of equality). |
However. we caution that some of this scatter is likely artificial: as we showed in de Grijs et al. ( | However, we caution that some of this scatter is likely artificial; as we showed in de Grijs et al. ( |
200041. 1ο age-extinction degeneracey is artificially worsened (in the sense that clusters ave artificially assigned. vounger ages) if re wavelength baseline used for the multi-parameter cluster SED analvsis lacks wavelength coverage loneward of the & iler. as is the case here. | 2003d), the age-extinction degeneracy is artificially worsened (in the sense that clusters are artificially assigned younger ages) if the wavelength baseline used for the multi-parameter cluster SED analysis lacks wavelength coverage longward of the $R$ filter, as is the case here. |
In. essence. this is shown by the enhanced population of the two youngest age bins (at + and S Myr) in Figs. | In essence, this is shown by the enhanced population of the two youngest age bins (at 4 and 8 Myr) in Figs. |
3bb and e for the models without restrictions on £(B12. | \ref{internal.fig}b b and c for the models without restrictions on $E(B-V)$. |
This situation can be avoided successfully by adopting a fixed. value for either the cluster population's (average) extinction or metallicity (de Cirijs et al. | This situation can be avoided successfully by adopting a fixed value for either the cluster population's (average) extinction or metallicity (de Grijs et al. |
2003d). | 2003d). |
Thus. in view of these considerations. this implies that our results are indeed: very comparable to those obtained from the OGLE-IL data. | Thus, in view of these considerations, this implies that our results are indeed very comparable to those obtained from the OGLE-II data. |
Finally. to assess the robustness of the individual ages. we compare the LMC cluster age determinations of L103 (uncorrected). OGLE-L and ourselves with those obtained for smaller cluster samples using a variety of techniques. | Finally, to assess the robustness of the individual ages, we compare the LMC cluster age determinations of H03 (uncorrected), OGLE-II and ourselves with those obtained for smaller cluster samples using a variety of techniques. |
In Fig. | In Fig. |
4 we have included those samples containing z5 clusters in common with our sample for which the authors determined their ages based. on. broac-banc photometry. | \ref{colours.fig} we have included those samples containing $\ge 5$ clusters in common with our sample for which the authors determined their ages based on broad-band photometry. |
With the exception of the Meurer et al. ( | With the exception of the Meurer et al. ( |
1990) results. who used the ultraviolet colours C1δ.31); and 605Bly. all other age determinations are. based. on blue. optical colours. | 1990) results, who used the ultraviolet colours $C(18-31)_0$ and $C(25-31)_0$, all other age determinations are based on blue optical colours. |
Dica et al. ( | Bica et al. ( |
1986. 1990) used the 6(42η vs. C(45 1L2)o vs. SWB tvpe (Searle. Wilkinson Bagnuolo 1980) diagnostics. while Chiosi et al. ( | 1986, 1990) used the $C(43-45)_0$ vs. $C(45-{\rm H}\beta)_0$ vs. SWB type (Searle, Wilkinson Bagnuolo 1980) diagnostics, while Chiosi et al. ( |
1988: CDV. clours) and Santos et al. ( | 1988; $UBV$ clours) and Santos et al. ( |
1995: (0By colours) limited themselves to the "standard set of broad-band Lilters. | 1995; $(U-B)_0$ colours) limited themselves to the “standard” set of broad-band filters. |
Although the Aleurer et al. ( | Although the Meurer et al. ( |
1990) ages are. clearly systematically greater than any of the ages determined by L103. OGLE-IEL or us. the other age determinations are statistically similar to those discussed. elsewhere in this paper. | 1990) ages are clearly systematically greater than any of the ages determined by H03, OGLE-II or us, the other age determinations are statistically similar to those discussed elsewhere in this paper. |
This is encouraging regarding the robustness of our results: the relatively large scatter is à side. cllect | This is encouraging regarding the robustness of our results; the relatively large scatter is a side effect |
threshold values even for very small flares. | threshold values even for very small flares. |
The MWSA was observed greater than 20 degrees for C-class flares. | The MWSA was observed greater than 20 degrees for C-class flares. |
For every B and A-class flare. MWSA was greater than 13 and 16 degrees respectively. | For every B and A-class flare, MWSA was greater than 18 and 16 degrees respectively. |
The MWSA again shows a similar evolutionary behavior as that of the SASSA. | The MWSA again shows a similar evolutionary behavior as that of the SASSA. |
The threshold values. however. were specific to the active region. | The threshold values, however, were specific to the active region. |
Thus. we conclude that the SASSA can be used as a reliable preclictor of maximum possible flux of X-ray flares. | Thus, we conclude that the SASSA can be used as a reliable predictor of maximum possible flux of X-ray flares. |
The data lor studying the evolution of SASSA in more active regions are not available for the time being. | The data for studying the evolution of SASSA in more active regions are not available for the time being. |
However. the inspection of the different [Iares which occurred in all the sunspots listed in the Table 1 of Tiwarietal.(2009b) show a similar trend. | However, the inspection of the different flares which occurred in all the sunspots listed in the Table 1 of \cite{tiw09b} show a similar trend. |
From the Table 1 of Tiwarietal.(2009b).. we also confirm a threshold value ol ~6 degrees for M-class flares as observed in our Figure 3(b). | From the Table 1 of \cite{tiw09b}, we also confirm a threshold value of $\sim$ 6 degrees for M-class flares as observed in our Figure 3(b). |
The peak flux of M-class flares associated with NOAA AR 10808 and NOAA AR 0959] are shown with their SASSA and MWSA values respectively by diamond svinbols in Figures 5(a) and 5(b). | The peak flux of M-class flares associated with NOAA AR 10808 and NOAA AR 09591 are shown with their SASSA and MWSA values respectively by diamond symbols in Figures 5(a) and 5(b). |
Figures 5(a) and 5(b) represent scatter plots between the peak GOES X-ray Πας and interpolated SASSA and MWSA values for that time. respectively. | Figures 5(a) and 5(b) represent scatter plots between the peak GOES X-ray flux and interpolated SASSA and MWSA values for that time, respectively. |
The cubic spline interpolation of the sample of the SASSA and the MWSA values has been done to get the SASSA and MWSA exactly at the time of peak fIux of the X-ray flare. | The cubic spline interpolation of the sample of the SASSA and the MWSA values has been done to get the SASSA and MWSA exactly at the time of peak flux of the X-ray flare. |
From the Figure 5(a). it can be noted that there is a good relationship between the | From the Figure 5(a), it can be noted that there is a good relationship between the |
(e.g..Sahaietal.1998:Mauroi1999:Iwoketal.2001:Hrivuak2001).. (Soker1991:Mastrodeimos&Morris1999:He2007:Exlgaretal. (ÀOLLisetal.2006)..nai | \citep[e.g.,][]{sah98, mau99,kwo01,hri01}. \citep{sok94,mas99,he07,edg08}. \citep{mor06}. \citet{kim07}. \citeauthor{ost99}' |
ta int Ixim&(2007).. Osrik.ers (1999) ps (Iximetal.2008).. (sim&Isin2009:Αι2010). | \citeyearpar{ost99} \citep{kim08}, \citep{kim09,kwt10}, \citep{nam10}. |
. (Namotui2010).. Ixim&Ivim(2009) referencestherein).. (sinu2011.heeafter11) rp M C51)ina “the int rírp=2M,!+1. 2tan.1((Mfr,A42—147. rj; | \citet{kim09} \citep[see][and references therein]{edg04}, \citep[hereafter \paper]
{kim11} $r_p$ $\mach_p$ $>$ $r/r_p=\varphi\mach_p^{-1}+1$ $2\tan^{-1}(\mach_p^2-1)^{1/2}$ $r_B$ \\ref{sec:simu} |
The recorded peak fluxes are not background-subtracted. | The recorded peak fluxes are not background-subtracted. |
A recent period of extremely low solar activity LLivingston Penn 2009: Salabert et 22009) has afforded a unique opportunity to study solar [ares occurring in individual active regions with low levels of background emission [rom other regions on the disk. | A recent period of extremely low solar activity Livingston Penn 2009; Salabert et 2009) has afforded a unique opportunity to study solar flares occurring in individual active regions with low levels of background emission from other regions on the disk. |
In this paper we examine a remarkable sequence of events in active region AR 11029 observed from 25 Oct 2009 (to 1 Nov 2009. | In this paper we examine a remarkable sequence of events in active region AR 11029 observed from 25 Oct 2009 to 1 Nov 2009. |
This small new-evele sunspot region. produced over 70 small solt X-ray flares in a clviaamic one-week burst of activity. during which (time it was the only [Iare-procducing active region on the Sun. | This small new-cycle sunspot region produced over 70 small soft X-ray flares in a dynamic one-week burst of activity, during which time it was the only flare-producing active region on the Sun. |
The absence of X-ray emission [rom other regions on the Sun at this time permits careful inspection of (he statistics of GOES events for the reeion. including background subtraction of the peak thax. | The absence of X-ray emission from other regions on the Sun at this time permits careful inspection of the statistics of GOES events for the region, including background subtraction of the peak flux. |
The kev question addressed here is whether a small. highly [Iare-procductive active region still exhibits a featureless power law in its [lare [requencesv-size distribution. or whether it is possible to identify a departure from the power law al large flare sizes. corresponding perhaps to the region containing a finite amount of energv. | The key question addressed here is whether a small, highly flare-productive active region still exhibits a featureless power law in its flare frequency-size distribution, or whether it is possible to identify a departure from the power law at large flare sizes, corresponding perhaps to the region containing a finite amount of energy. |
It is also of interest to examine the waiting-time distribution for such a region. again taking advantage of the low levels of background. emission. (o see how the flaring rate varies in (ime. | It is also of interest to examine the waiting-time distribution for such a region, again taking advantage of the low levels of background emission, to see how the flaring rate varies in time. |
The sections of the paper are divided as follows. | The sections of the paper are divided as follows. |
Section 2 describes the observations of the region. | Section 2 describes the observations of the region. |
Section 3 presents analvsis. with section 3.1 describing the procedure of backeround subtraction of the peak fIuxes. aud sections 3.2 and 3.3 describing (he analysis and modeling of the Lequeney-peak flux. distribution and (he waiting-time distribution respectively. | Section 3 presents analysis, with section 3.1 describing the procedure of background subtraction of the peak fluxes, and sections 3.2 and 3.3 describing the analysis and modeling of the frequency-peak flux distribution and the waiting-time distribution respectively. |
Section 4 discussed (he results. aud the appendices present the methods of Bavesian inference for a power law and for a power law with an upper rollover used in section 3.2. | Section 4 discussed the results, and the appendices present the methods of Bayesian inference for a power law and for a power law with an upper rollover used in section 3.2. |
Solar active region AR 11029 emerged on the disk on 2122 Oct 2009 and developed sunspols on 24 Oct. Figure 1 shows a sequence of daily Global Oscillations Network Group (GONG) magnetogranms for that period of time and illustrates the emergence of the region and ils rapid evolution. | Solar active region AR 11029 emerged on the disk on 21–22 Oct 2009 and developed sunspots on 24 Oct. Figure 1 shows a sequence of daily Global Oscillations Network Group (GONG) magnetograms for that period of time and illustrates the emergence of the region and its rapid evolution. |
The region grew in size ancl magnetic complexity. as il crossed the disk. arriving al the west limb on 1 Nov. However the region remained relatively small: the sunspot areas recorded. in the US National Weather Service/National Oceanic and Atmospheric Administration (NWS/NOAA) Solar Region | The region grew in size and magnetic complexity as it crossed the disk, arriving at the west limb on 1 Nov. However the region remained relatively small: the sunspot areas recorded in the US National Weather Service/National Oceanic and Atmospheric Administration (NWS/NOAA) Solar Region |
the general structure of the BLR aud continua cluitting region. | the general structure of the BLR and continuum emitting region. |
Table 2 shows that L3190 icrοσον as objects are secu more pole-on: by a factor of 2 for high Eddington ratio objects iux by a factor of 3 for low Eddinetou ratio objects. | Table 2 shows that $_{5100}$ increases as objects are seen more pole-on: by a factor of 2 for high Eddington ratio objects and by a factor of 3 for low Eddington ratio objects. |
I> width is not stronely depeudeut ou oricutaion for high Eddington ratio objects. but for low Eddington ratio objects. it is larger by :O11 in those objects seen edge-on. | $\beta$ width is not strongly dependent on orientation for high Eddington ratio objects, but for low Eddington ratio objects, it is larger by about in those objects seen edge-on. |
Consistent with the Risalipotal.(2011). study. is muallr i pole-on objects than in edee-onu LEWioobjects. though the effect is nmmeh less than would be expected if © III CLUISSIOLL were isotropic. aud the decrease were due only to the increase in the apparent contmnuuni hDmunuinosity. | Consistent with the \citet{ris11} study, $_{[O III]}$ is smaller in pole-on objects than in edge-on objects, though the effect is much less than would be expected if [O III] emission were isotropic, and the decrease were due only to the increase in the apparent continuum luminosity. |
Similarly. the |O ITI] outflows also secu to broaden the [O TH) lines. greatly in the high Eddington ratio objects (bv definition). but slightly even iu the low LEddiusetou ratio objects. while uo such effect is seen in the |O TT lines, | Similarly, the [O III] outflows also seem to broaden the [O III] lines, greatly in the high Eddington ratio objects (by definition), but slightly even in the low Eddington ratio objects, while no such effect is seen in the [O II] lines. |
Overall. a picture consistent with these findings Is as follows. | Overall, a picture consistent with these findings is as follows. |
The cout ds eluitted frou the surtace of a isk aud the BLR is somewhat flattened also. | The continuum is emitted from the surface of a disk and the BLR is somewhat flattened also. |
At veh ER. both of these regions are less flattened ini at ow ER. | At high ER, both of these regions are less flattened than at low ER. |
The Fe I inflow. see niu ow ER objects. is roughly in the plane of this cisk. though it nav be that in edge-on objects. We see d at ascep angele. but not zero degrees sccatise of the coplanar obscuring torus. | The Fe II inflow, seen in low ER objects, is roughly in the plane of this disk, though it may be that in edge-on objects, we see it at a steep angle, but not zero degrees because of the coplanar obscuring torus. |
Perpendicular to his disk is the biconical outflow of the narrow foriddenu lines. | Perpendicular to this disk is the biconical outflow of the narrow forbidden lines. |
In high ER objects. we see the |O TIT coming towards us when our view is pole-ou. | In high ER objects, we see the [O III] coming towards us when our view is pole-on. |
Lower ionization species probally arise further out where 16 flow has decelerated. | Lower ionization species probably arise further out where the flow has decelerated. |
Estimates of the effec of orieutation on L3100 alc FWIINM IL) allow a) assessneut of its impact Ol derived quantiticSÀN pu ad Lou gu. | Estimates of the effect of orientation on $_{5100}$ and FWHM $\beta$ allow an assessment of its impact on derived quantities $_{BH}$ and $_{bol}$ $_{Edd}$. |
Most of the effect appears to be on Iunuinositv. where a facor of 2-3 betwee 1ec-onu aud pole-ou objects traslates iuto a slüf iu both Mp aud ER of to a factor of about 2 | Most of the effect appears to be on luminosity, where a factor of 2-3 between edge-on and pole-on objects translates into a shift in both $_{BH}$ and ER of to a factor of about 2. |
The effect ou line width. apyxurentlv sieuificaut oily for low Eddineton ratio oly]ects. translates 1ito an increase of about iu calculated Moy for edge-on objects. but iu the opposite seuse O he bhuuinositv effect. | The effect on line width, apparently significant only for low Eddington ratio objects, translates into an increase of about in calculated $_{BH}$ for edge-on objects, but in the opposite sense to the luminosity effect. |
It is possible that the line width effect is substantially larecr han is seen in this sample. since the objects with verv broad IL) lines are known to have relatively weak Fe ID cuaission. aud so have been prefercutially excluded from the [hietal.(2008) saluple. | It is possible that the line width effect is substantially larger than is seen in this sample, since the objects with very broad $\beta$ lines are known to have relatively weak Fe II emission, and so have been preferentially excluded from the \citet{hu08} sample. |
If the quantitative differences between subsets are used to correct cach subset to an average orientation. the corrections change the May aud Loj/Lg;; unnbers by a few tens of percent. | If the quantitative differences between subsets are used to correct each subset to an average orientation, the corrections change the $_{BH}$ and $_{bol}$ $_{Edd}$ numbers by a few tens of percent. |
Thev bring the pa values closer for simular objects at different orieutatious. | They bring the $_{BH}$ values closer for similar objects at different orientations. |
The uch and low Eddington ratio subsets retain the same relationship: the Lhieh Eddinetom ratio objects have 2 - 3 times the Eddineton ratio value of the low Eddington ratio objects. | The high and low Eddington ratio subsets retain the same relationship; the high Eddington ratio objects have 2 - 3 times the Eddington ratio value of the low Eddington ratio objects. |
This work is a first step towards πιοται orientation effects based on the inflow aud outflow volocities in large samples. | This work is a first step towards understanding orientation effects based on the inflow and outflow velocities in large samples. |
Several questions that represent possible next steps are: l. | Several questions that represent possible next steps are: 1. |
For objects without strong Fe IL can the asvuuuetrv of the ID) line be used to ideutity objects that are secu close to edge-on? | For objects without strong Fe II, can the asymmetry of the $\beta$ line be used to identify objects that are seen close to edge-on? |
2. | 2. |
Can a sufficiently complete aud. well-defiued suuple of objects be analyzed iu this wav to separate oricutation-driven aud Eddington driven trends with higher precision? | Can a sufficiently complete and well-defined sample of objects be analyzed in this way to separate orientation-driven and Eddington ratio-driven trends with higher precision? |
3. | 3. |
Does a correction to Mp; based ou oricutation have the effect of reducing the scatter in the τρ σι relation or of clarifviug the location of Narrow -Line Sevfert Ls in that diagram? | Does a correction to $_{BH}$ based on orientation have the effect of reducing the scatter in the $_{BH}$ $\sigma_{\star}$ relation or of clarifying the location of Narrow -Line Seyfert 1s in that diagram? |
1. | 4. |
Can trends in other properties. for example. the shape of the line. be shown to correlate with orientation. in order to provide additional information about the structure or kinematics of the inner regions of QSOs? | Can trends in other properties, for example, the shape of the $\beta$ line, be shown to correlate with orientation, in order to provide additional information about the structure or kinematics of the inner regions of QSOs? |
Ithauk Luiei Foschini aud the organizers of the confercuceUniverse. held in Mili. Italy in Apri 2011 for the iuvitation that led to this work. | I thank Luigi Foschini and the organizers of the conference, held in Milan, Italy in April 2011 for the invitation that led to this work. |
I hawks Wermine Laudt. Guido Risaliti. aud Alessandro Marconi for helpful discussions. | I thank Hermine Landt, Guido Risaliti, and Alessandro Marconi for helpful discussions. |
Spectroscopic and. photometric observations. reveal that globular clusters host multiple. stellar. populations. | Spectroscopic and photometric observations reveal that globular clusters host multiple stellar populations. |
. Spectroscopic studies show. star-to-sbar variations dn the abundances of light elements. such as Na. O. AL and Ale. indicating that a significant fraction. (50-S0%)) of elobular cluster stars must. have. formed. out. of. matter processed through a high-temperature CNO evcle in a first eencration (hereafter FC.) of stars (see e.g. Carretta ct al. | Spectroscopic studies show star-to-star variations in the abundances of light elements, such as Na, O, Al, and Mg, indicating that a significant fraction ) of globular cluster stars must have formed out of matter processed through a high-temperature CNO cycle in a first generation (hereafter FG) of stars (see e.g. Carretta et al. |
2009a. 2009b and references therein). | 2009a, 2009b and references therein). |
Photometric studies reveal the presence of multiple main sequences. subgiant. and rec-eiant branches in numerous clusters. supporting the spectroscopic. evidence for multiple populations (sce ee. Piotto 2009 ancl references. therein). | Photometric studies reveal the presence of multiple main sequences, subgiant, and red-giant branches in numerous clusters, supporting the spectroscopic evidence for multiple populations (see e.g. Piotto 2009 and references therein). |
Photometric measurements also provide evidence for a population of very Le-rich stars among the second-generation. (hereafter SC) stars of some clusters (sec c.g. Piotto et al. | Photometric measurements also provide evidence for a population of very He-rich stars among the second-generation (hereafter SG) stars of some clusters (see e.g. Piotto et al. |
2007). | 2007). |
These findings confirm the predictions of previous stuclics (D'Xntona et al. | These findings confirm the predictions of previous studies (D'Antona et al. |
2002: D'Antona Caloi 2004. D'Antona Caloi 2008) that suggested the existence of a population of stars with a strong He enhancement on the basis of the extension. of the horizontal∙⊀ branch. | 2002; D'Antona Caloi 2004, D'Antona Caloi 2008) that suggested the existence of a population of stars with a strong He enhancement on the basis of the extension of the horizontal branch. |
∙ Phe origin of. the gas out of which SG stars formed. is still an open question: in addition to the scenario involving AGB stars (Cottrell Da Costa 1981. Ventura et al. | The origin of the gas out of which SG stars formed is still an open question: in addition to the scenario involving AGB stars (Cottrell Da Costa 1981, Ventura et al. |
2001) described in more detail below. possible gas sources proposed in the literature also include rapiclly rotating massive stars ancl massive binary stars (Decressin et. al. | 2001) described in more detail below, possible gas sources proposed in the literature also include rapidly rotating massive stars and massive binary stars (Decressin et al. |
2007. De Mink et al. | 2007, De Mink et al. |
2009: see also Renzini 2008 ancl references therein for a review). | 2009; see also Renzini 2008 and references therein for a review). |
Alany fundamental questions concerning. globular cluster star formation and cluster chemical ancl dynamical history are raised by the discovery of multiple populations. and are targets of ongoing investigations (see e.g. DErcole et al. | Many fundamental questions concerning globular cluster star formation and cluster chemical and dynamical history are raised by the discovery of multiple populations, and are targets of ongoing investigations (see e.g. D'Ercole et al. |
2008. 2010. Vesperini ct al. | 2008, 2010, Vesperini et al. |
2010. Bekki 2011 ancl references therein). | 2010, Bekki 2011 and references therein). |
D'Ercole et abo ( | D'Ercole et al. ( |
2008) explored the formation and. dynamical evolution of multiple populations in elobular cluster by means of hydrodynamical and N-body simulations. focusing on a model in which SCG stars form from the ejecta of FG: AGB stars. | 2008) explored the formation and dynamical evolution of multiple populations in globular cluster by means of hydrodynamical and N-body simulations, focusing on a model in which SG stars form from the ejecta of FG AGB stars. |
Our simulations show that | Our simulations show that |
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