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At the very least. it is clear that these E+A galaxies found in the field region cannot be explained by a physical mechanism that works in the cluster region. | At the very least, it is clear that these E+A galaxies found in the field region cannot be explained by a physical mechanism that works in the cluster region. |
E+A galaxies have been often thought to be transition objects during the cluster galaxy evolution such as the Butcher-Oemler effect (e.g.. Goto et al. | E+A galaxies have been often thought to be transition objects during the cluster galaxy evolution such as the Butcher-Oemler effect (e.g., Goto et al. |
2003b). the morphology-density relation (e.g.. Goto et al. | 2003b), the morphology-density relation (e.g., Goto et al. |
2003c: Goto et al. | 2003c; Goto et al. |
2004). and the correlation between various properties of galaxies. with the. environment (e.g. Tanaka et al. | 2004), and the correlation between various properties of galaxies with the environment (e.g. Tanaka et al. |
2004). | 2004). |
However. explaining cluster galaxy evolution using E+A galaxies may not be realistic anymore. | However, explaining cluster galaxy evolution using E+A galaxies may not be realistic anymore. |
Alternatively. galaxy-galaxy interaction has been known to trigger star formation in the pair of galaxies (Schweizer 1982: Lavery Henry 1988; Liu Kennicutt 1995a.b: Schweizer 1996). | Alternatively, galaxy-galaxy interaction has been known to trigger star formation in the pair of galaxies (Schweizer 1982; Lavery Henry 1988; Liu Kennicutt 1995a,b; Schweizer 1996). |
Oegerle. Hill. Hoessel(1991) found a nearby E+A galaxy with a tidal feature. | Oegerle, Hill, Hoessel(1991) found a nearby E+A galaxy with a tidal feature. |
High resolution imaging of Hubble Space Telescope supported the galaxy-galaxy interaction scenario by identifying that some of post-starburst (E+A) galaxies in high redshift clusters show disturbed or interacting signatures (Couch et al. | High resolution imaging of Hubble Space Telescope supported the galaxy-galaxy interaction scenario by identifying that some of post-starburst (E+A) galaxies in high redshift clusters show disturbed or interacting signatures (Couch et al. |
1994.1998: Dressler et al 1994: Oemler. Dressler. Butcher 1997). | 1994,1998; Dressler et al 1994; Oemler, Dressler, Butcher 1997). |
Liu Kennicutt (1995a.b) observed 40 merging/interacting systems and found that some of their spectra resemble E+A galaxies. | Liu Kennicutt (1995a,b) observed 40 merging/interacting systems and found that some of their spectra resemble E+A galaxies. |
Bekki. Shioya. Couch (2001) modeled galaxy-galaxy mergers with dust extinction. confirming that such systems can produce spectra which evolve into E+A spectra. | Bekki, Shioya, Couch (2001) modeled galaxy-galaxy mergers with dust extinction, confirming that such systems can produce spectra which evolve into E+A spectra. |
Recently. GO3 found that young E+A galaxies have 8 times more companion galaxies within 50 kpe. providing a strong support for the merger/interaction origin of E+A galaxies. | Recently, G03 found that young E+A galaxies have 8 times more companion galaxies within 50 kpc, providing a strong support for the merger/interaction origin of E+A galaxies. |
However. an important issue remains to be addressed on the origin of E+A galaxies. | However, an important issue remains to be addressed on the origin of E+A galaxies. |
E+A galaxies may beexplained | E+A galaxies may beexplained |
What is shehtlv more puzzling is (hat three asteroids with 108 MOID values in the lunar distance also have /?(20.0.5)<54. | What is slightly more puzzling is that three asteroids with B10's MOID values in the lunar distance also have $P(20,0.5)<5$. |
. One of these is classified as S (719 Albert). and {wo are Qs (162058 1997AEI2 and 2008CLI). | One of these is classified as S (719 Albert), and two are Qs (162058 1997AE12 and 2008CL1). |
This shows that the classification of objects based on MOID is ambiguous because it does not properly take into account the. actual encounter probability over a finite time interval. | This shows that the classification of objects based on MOID is ambiguous because it does not properly take into account the actual encounter probability over a finite time interval. |
It is therefore incorrect (ο assign the DIO's result (even approximate) statistical sienilicance. because such a calculation will depend on (he subjective choice of (he cutoff value. | It is therefore incorrect to assign the B10's result (even approximate) statistical significance, because such a calculation will depend on the subjective choice of the cutoff value. |
For example. the partition of Q-tvpe objects between D(20.0.5)>5254 and P(20.0.5)«5% is nol statistically unusual (unless MDBAs were taken into When only encounters to the Earth are considered. the classification of objects based on their encounter probability becomes less ambiguous (Fig. 3)). | For example, the partition of Q-type objects between $P(20,0.5)>5$ and $P(20,0.5)<5$ is not statistically unusual (unless MBAs were taken into When only encounters to the Earth are considered, the classification of objects based on their encounter probability becomes less ambiguous (Fig. \ref{dprob}) ). |
This happens because the probability of Earth encounter is a step-like function with either (20.0.5)>LOY or D(20.0.5)<19. and very [ew objects (6 in total: 3288. 5143. GOLT. 23187. 2O0GNAI and SOOLFAL) in the intermediate range. | This happens because the probability of Earth encounter is a step-like function with either $P(20,0.5)>10$ or $P(20,0.5)<1$, and very few objects (6 in total; 3288, 5143, 6047, 23187, 2006NM and 2001FA1) in the intermediate range. |
One of these six intermediate objects. 5143 IHeracles. is a Q with an Earth-encounter probability P(20.0.5)=9%. | One of these six intermediate objects, 5143 Heracles, is a Q with an Earth-encounter probability $P(20,0.5)=9$. |
. Our 20 objects with also have large MOID for Earth encounters according to DIO. | Our 20 objects with $P(20,0.5)<1$ also have large MOID for Earth encounters according to B10. |
We will consider two cases in the following text. | We will consider two cases in the following text. |
In the first case. we will assume that the main effect on surface regolith of an asteroid is driven by tidal gravity during the asteroids encounters to the terrestrial planets (case 1). | In the first case, we will assume that the main effect on surface regolith of an asteroid is driven by tidal gravity during the asteroid's encounters to the terrestrial planets (case 1). |
All planets. mainly Venus and Earth. must be considered in this case. | All planets, mainly Venus and Earth, must be considered in this case. |
To compare our models with the data. all 95 objects with known near] taxonomy will be considered as one group. | To compare our models with the data, all 95 objects with known near-IR taxonomy will be considered as one group. |
In the second case. we will consider encounters to (he Earth only (case 2). | In the second case, we will consider encounters to the Earth only (case 2). |
There is a possibility (discussed in more detail in $55) that electrically charged regolith particles (e.g.. bv photoelectric effect: Lee 1996) can be lofted by the Lorentz force when the asteroid passes through the Earth's magnetosphere. | There is a possibility (discussed in more detail in 5) that electrically charged regolith particles (e.g., by photoelectric effect; Lee 1996) can be lofted by the Lorentz force when the asteroid passes through the Earth's magnetosphere. |
since (he Earth magnetosphere extends (o a larger distance (han where tidal gravity could be important. its effects may potentially be relevant for distant encounters. | Since the Earth magnetosphere extends to a larger distance than where tidal gravity could be important, its effects may potentially be relevant for distant encounters. |
Distant encounters with Venus and Murs need not to be considered because these planets do not have important magnetic fields. | Distant encounters with Venus and Mars need not to be considered because these planets do not have important magnetic fields. |
In this case. we will discard 20 objects with P(20.0.5)<14 for Earth encounters (group 2 in the following) from our list aud consider the remaining 75 objects onlv (group 1). | In this case, we will discard 20 objects with $P(20,0.5)<1$ for Earth encounters (group 2 in the following) from our list and consider the remaining 75 objects only (group 1). |
The SW timescale and critical encounter distance for which the tidal gravity (or Lorentz force) can be important are treated. as free. parameters in (he following. | The SW timescale and critical encounter distance for which the tidal gravity (or Lorentz force) can be important are treated as free parameters in the following. |
Specilicallv. we determine the number of bodies in the selected sample Chat are expected to have atleast one encounter with distance r«r* in lime /. where / and r are ου parameters. | Specifically, we determine the number of bodies in the selected sample that are expected to have atleast one encounter with distance $r<r^*$ in time $t$, where $t$ and $r^*$ are free parameters. |
This value eives us a sense of the expected fraction of the Q-(vpe objects in our model as a function of the SW timescale and r*.? As in DIO. we use a definition of the SW Umescale. (oy. as the characteristic time interval | This value gives us a sense of the expected fraction of the Q-type objects in our model as a function of the SW timescale and $r^*$ As in B10, we use a definition of the SW timescale, $t_{\rm sw}$ , as the characteristic time interval |
Once the iducial stars were characterized. a conputer progam collated the DAOPHOT image centers [rom he original pictures. aud generatec a master raw data file coutainiug the fixed information alyout the measwed stars. the celestial location. he Julian dates of the exposures. and the meastred image ceners (ολο.ολο) From all the picures. | Once the fiducial stars were characterized, a computer program collated the DAOPHOT image centers from the original pictures, and generated a master raw data file containing the fixed information about the measured stars, the celestial location, the Julian dates of the exposures, and the measured image centers $(x_{\rm DAO}, y_{\rm DAO})$ from all the pictures. |
Iu addition. a weight of zero Or One was assigned to each star indicating whetller it was to be used in generating coordinate transformations. | In addition, a weight of zero or one was assigned to each star indicating whether it was to be used in generating coordinate transformations. |
The progra1 star was never used for the coodlinate trausformations. and other stars were eliniiuated from tie transformations if preliminary analysis showed large scatter or (in some cases) la‘ee proper noious or parallaxes. | The program star was never used for the coordinate transformations, and other stars were eliminated from the transformations if preliminary analysis showed large scatter or (in some cases) large proper motions or parallaxes. |
The analysis proceeded iu several steps as follows: For each star. corrections for differential refraction. differential aberration. aud DCR were computed. in the (Xgq.Yaa) system. | The analysis proceeded in several steps as follows: For each star, corrections for differential refraction, differential aberration, and DCR were computed, in the $X_{\rm
fid}, Y_{\rm fid}$ ) system. |
A transformation was derived between Gepao. po) aud (Nga. Yga). | A transformation was derived between $x_{\rm DAO}, y_{\rm DAO}$ ) and $X_{\rm fid}, Y_{\rm
fid}$ ). |
The uet correction was transformed back to the Grpxo-upao! system. and added to the original coordinates. | The net correction was transformed back to the $x_{\rm DAO}, y_{\rm
DAO}$ ) system, and added to the original coordinates. |
Thus the coorcitales were "born corrected’. | Thus the coordinates were `born corrected'. |
Routines adapted from perlormed the spherical trigonometrye calculations. | Routines adapted from performed the spherical trigonometry calculations. |
Tests showed that with he exception of DCR (cdiscussed below). these correctious generally mace relatively little dillerence o the results. because their effects were largely absorbed by the ‘plate model later in the process. | Tests showed that with the exception of DCR (discussed below), these corrections generally made relatively little difference to the results, because their effects were largely absorbed by the `plate model' later in the process. |
The DCR correction calls for some discussion. | The DCR correction calls for some discussion. |
Early experimeuts with fields deliberately taken oth near and far (rom the merician suggested a DCR coefficient near 7 mas per uuit (aus) per iit (V—£). whereas the polynomial given by USNO92 implies a value of 29 in the samme units or tlieir broader passbaud. | Early experiments with fields deliberately taken both near and far from the meridian suggested a DCR coefficient near 7 mas per unit $\tan z$ ) per unit $(V - I)$, whereas the polynomial given by USNO92 implies a value of 29 in the same units for their broader passband. |
E checked. the empirically-derived DCR coefficient. using a procedure outlined by Gubler&Tytler(1998).. as follows. | I checked the empirically-derived DCR coefficient using a procedure outlined by \citet{gublertytler}, as follows. |
Library spectra [rom Pickles(1908) were convolve with passbaucs from Bessell(1990) to compute effective wavelengths as a funetion of V—£. aux aslalib (Wallace1991) routine was used to to find the refraction as a function of wavelength. | Library spectra from \citet{pickles} were convolved with passbands from \citet{bessell} to compute effective wavelengths as a function of $V - I$, and a \citep{wallace} routine was used to to find the refraction as a function of wavelength. |
The final result was 2 mas per uuit (tan z) per unit (V—4. in reasonable agreement with the empirica T. | The final result was 5 mas per unit $\tan z$ ) per unit $(V-I)$, in reasonable agreement with the empirical 7. |
To verify the procedure. the calculation was repeated for the USNO92 passbaxl Capproxiuiatec as flat across their coverage). aud their value of 29 uiits was recovered successfully. | To verify the procedure, the calculation was repeated for the USNO92 passband (approximated as flat across their coverage), and their value of 29 units was recovered successfully. |
The CrpAO- /pAO) coordiuates were trauslormed to the system outline by (Nga. Via). using a four-coustart plate model (wuch allows oulv shifts in zero point. a rigk rotation. aud a scale chauge). | The $x_{\rm DAO}, y_{\rm DAO}$ ) coordinates were transformed to the system outlined by $X_{\rm fid},Y_{\rm fid}$ ), using a four-constant plate model (which allows only shifts in zero point, a rigid rotation, and a scale change). |
These positious were averaged to create refined positious (μας.Yao for each star. | These positions were averaged to create refined positions $X_{\rm fid2}, Y_{\rm fid2}$ ) for each star. |
The errors in these positious were much reduced. because of averaging over many frames and because of the previous step's removal of computable offsets. | The errors in these positions were much reduced because of averaging over many frames and because of the previous step's removal of computable offsets. |
The 1‘ausformatious between Crpo- ypo) aud the IXY system were computed again using CXgq. Yao) as the target coordinates and using a more flexible plate moclel of the form | The transformations between $x_{\rm DAO}, y_{\rm DAO}$ ) and the $XY$ system were computed again using $X_{\rm fid2}, Y_{\rm fid2}$ ) as the target coordinates and using a more flexible plate model of the form |
Ambipolar diffusion is the joint drift. of charged. particles and the associated magnetic Dux with respect to the neutral particles in a partially ionizecl plasma. | Ambipolar diffusion is the joint drift of charged particles and the associated magnetic flux with respect to the neutral particles in a partially ionized plasma. |
Alestel&Spitzer(1956) first. proposed. it in order to explain the loss of magnetic [lux from the dense cores of molecular clouds. required. for the formation of stars. starting an active field of research in this area. | \citet{MestelSpitzer56}
first proposed it in order to explain the loss of magnetic flux from the dense cores of molecular clouds, required for the formation of stars, starting an active field of research in this area. |
Later. it was suggested to also play a role in the decay. of the magnetic fields of neutron stars (JonesLOST:Llarrison1991:Pethick1992:Goldre-ich<eisenegger. 1992... hereafter. GR-92) which became particularly relevant with the identification of “magnetars”. neutron stars whose main power source appears to be the dissipation of their magnetic field 2004). | Later, it was suggested to also play a role in the decay of the magnetic fields of neutron stars \citealp{J-87,H-91,P-92,GR-92}, hereafter GR-92) which became particularly relevant with the identification of “magnetars”, neutron stars whose main power source appears to be the dissipation of their magnetic field \citep{DT-92,TD-96,ACT-04}. |
. In a previous paper2008:: hereafter Paper D). we established a multilluid ormalism. in which it is possible to study the. long-erm evolution. of magnetic fields in neutron stars (sec telsenegger2009 for a discussion of the main properties of the magnetic field equilibria and. their subsequent long-erm evolution). | In a previous paper; hereafter Paper I), we established a multifluid formalism in which it is possible to study the long-term evolution of magnetic fields in neutron stars (see \citealt{R-09} for a discussion of the main properties of the magnetic field equilibria and their subsequent long-term evolution). |
In that work. and [following the ideas developed. by. €iH-92.. we included. the effects. of several ohvsical processes that are also relevant for star formation ancl protoplanetary. disks. includingdiffusion.diiff (non-dissipative advection of the magnetic field w the associated electrical. current). ancl (clissipation of currents through the electrical resistivity) | In that work, and following the ideas developed by GR-92, we included the effects of several physical processes that are also relevant for star formation and protoplanetary disks, including, (non-dissipative advection of the magnetic field by the associated electrical current), and (dissipation of currents through the electrical resistivity). |
llere. we continue this study and concentrate our analvsis on the long-term evolution of the magnetic field caused by ambipolar dilfusion. aided. by beta decavs. | Here we continue this study and concentrate our analysis on the long-term evolution of the magnetic field caused by ambipolar diffusion aided by beta decays. |
Following the same philosophy of Paper 1. and as a first approach to the understanding of our general formalism. we focus on a simplified. one-dimensional configuration in which the magnetic field pointsin one Cartesian direction z but varies only along an orthogonal direction wv. i. e.. B= Bore. | Following the same philosophy of Paper I, and as a first approach to the understanding of our general formalism, we focus on a simplified, one-dimensional configuration in which the magnetic field pointsin one Cartesian direction $z$ but varies only along an orthogonal direction $x$ , i. e., $\vec B=B(x,t)\hat z$ . |
Such models have also been considered in several | Such models have also been considered in several |
Fields. | Fields. |
The results are: aud Our selection of the sample of the stars representing the RGB is eutirely motivated by our choice of the absolute calibration of the RGB tip. | The results are: and Our selection of the sample of the stars representing the RGB is entirely motivated by our choice of the absolute calibration of the RGB tip. |
This approach actually lits the analysis to about 20 of the total umber of available RGB stars. | This approach actually limits the analysis to about 20 of the total number of available RGB stars. |
As an alternative approach. one could choose to adopt a immch larger saunple of RGB stars. reaching the liehanetallicity edee of the RGB. | As an alternative approach, one could choose to adopt a much larger sample of RGB stars, reaching the high-metallicity edge of the RGB. |
We argue that this approach would provide consistent results. but with a lower precision. | We argue that this approach would provide consistent results, but with a lower precision. |
This is shown in Figure 10.. | This is shown in Figure \ref{ferraro2.ps}. |
Tn this Figure we plot the CMD of NGC 300. Field 2. in the absolute plane. using the distance aud the reddening provided by Ciüerenetal.(2005).. | In this Figure we plot the CMD of NGC 300, Field 2, in the absolute plane, using the distance and the reddening provided by \citet{2005ApJ...628..695G}. |
The continuous line shows the color dependence of the RGB tip according to Bellazzinictal. (2001).. | The continuous line shows the color dependence of the RGB tip according to \citet{2001ApJ...556..635B}. |
It is evident that the slope of the functiou MPROBOSI) reproduces very closely the observed data. | It is evident that the slope of the function $M_I^{TRGB} vs. (V-I)_0$ reproduces very closely the observed data. |
Ou the other hand. usine the Helvuetallicity part of the CMD would introduce additional errors due the still wucertain slope of he lhieh-nctallicity extension of the calibration. | On the other hand, using the high-metallicity part of the CMD would introduce additional errors due the still uncertain slope of the high-metallicity extension of the calibration. |
Another issue that should be given attention ο is the age of the uuderlviug population used o define the RGB sample. | Another issue that should be given attention to is the age of the underlying population used to define the RGB sample. |
Whenever the RGB ip technique is applied to a composite stellar »pulatiou. the possibility of biases arises. due o the fact that the presence of a well-developed and populated RGB does not necessarily Πρίν he presence of a globular chister-lke population. while the calibration of the absolute magnitude of the RGB tip relics completely on a sample of elobular clusters. | Whenever the RGB tip technique is applied to a composite stellar population, the possibility of biases arises, due to the fact that the presence of a well-developed and populated RGB does not necessarily imply the presence of a globular cluster-like population, while the calibration of the absolute magnitude of the RGB tip relies completely on a sample of globular clusters. |
Barkeretal.(2001) reporte i. the RGB distances are rather museusitive to 16 stellar populations provided most of the stars are more nietal poor than |Fe/Il]=—0.3 aux iat there is not a strong star formation burst )etween L aud 2 Cyr. | \citet{2004ApJ...606..869B} reported that the RGB distances are rather insensitive to the stellar populations provided most of the stars are more metal poor than $\rm{[Fe/H]}=-0.3$ and that there is not a strong star formation burst between 1 and 2 Gyr. |
Salaris&Cirardi(2005) extended this analysis to real cases. aud show iat applving the standard technique for RGD tip distances to the LAIC aud to the SAIC could result | \citet{2005MNRAS.357..669S} extended this analysis to real cases, and showed that applying the standard technique for RGB tip distances to the LMC and to the SMC could result |
The full set of derived abundances. together with the original numbers derived by Rónnback&Bergvall(1995).. is presented in Table 2.. | The full set of derived abundances, together with the original numbers derived by \citet{Ronnback95}, is presented in Table \ref{abundances}. |
We estimate the typical error (mainly due to the method itself) in abundances derived using the NS- and ON-calibrations to be 40.1 dex. and the 7.-based abundances is expected to have slightly smaller total errors. | We estimate the typical error (mainly due to the method itself) in abundances derived using the NS- and ON-calibrations to be $\pm 0.1$ dex, and the $T_{\rm e}$ -based abundances is expected to have slightly smaller total errors. |
The T.-based abundances agree very well with the abundances derived by Rónnback.&Bergvall(1995.seealsoFigs.1. and 2 in the presentpaper). | The $T_{\rm e}$ -based abundances agree very well with the abundances derived by \citet[][see also Figs. \ref{OHcomp} and \ref{OHNO} in the present. |
Among the galaxies with detectable [O NT].14363-lines. the lowest Z.-based oxygen abundance is found in ESO 489-656 where I2+logtO/H)=7.47 (7.49accordingtoRónnback&Bergvall 1995). | Among the galaxies with detectable ${\rm [O~{\textsc III}]} \lambda 4363$ -lines, the lowest $T_{\rm e}$ -based oxygen abundance is found in ESO 489-G56 where $12+\log({\rm O/H}) = 7.47$ \citep[7.49 according to][]{Ronnback95}. |
. In fact. we have only been able to find one LSBG with lower 7.-based oxygen abundance when searching the literature (CGCG269-049,logtO/H»2003). | In fact, we have only been able to find one LSBG with lower $T_{\rm e}$ -based oxygen abundance when searching the literature \citep[CGCG 269-049, $\log({\rm O/H}). |
The ON-abundances also agree with the 7.-based abundances as well as with the NS-abundances and the existence of a at low metallicity (see Fig. 2). | The ON-abundances also agree with the $T_{\rm e}$ -based abundances as well as with the NS-abundances and the existence of a at low metallicity (see Fig. \ref{OHNO}) ). |
There is essentially only one exception: H region B in ESO 158-G15 which has a significantly ower N/O-ratio than the rest of the samplecalibration. | There is essentially only one exception: H region B in ESO 158-G15 which has a significantly lower N/O-ratio than the rest of the sample. |
This may be due to the fact that the N»-value for his object lies on the boundary between the cool and warm regimes in the NS- and ON-calibrations. Among he oxygen abundances derived using the NS- and ON-calibrations we find one particular H region with a very low abundance. | This may be due to the fact that the $N_2$ -value for this object lies on the boundary between the cool and warm regimes in the NS- and ON-calibrations, Among the oxygen abundances derived using the NS- and ON-calibrations we find one particular H region with a very low abundance. |
This is discussed in detail below. | This is discussed in detail below. |
Among the galaxies in this study. ESO 546-G3+ stands out as the most metal poor according to our analysis Previous empirical estimates of the oxygen abundances in two of the three observed Η t--regions were significantly higher (RGnnback&Bergvall1995). which was likely due to use of ill-determined strong-line calibrations (not suitable for very low metallicities). | Among the galaxies in this study, ESO 546-G34 stands out as the most metal poor according to our analysis Previous empirical estimates of the oxygen abundances in two of the three observed H -regions were significantly higher \citep{Ronnback95}, which was likely due to use of ill-determined strong-line calibrations (not suitable for very low metallicities). |
However. it was noted that the Skillman(1989) calibration derived for metal-poor systems gave | However, it was noted that the \citet{Skillman89} calibration derived for metal-poor systems gave |
and large fluctuations in time. | and large fluctuations in time. |
The ratio of small to large-scale magnetic field remains small, and decreases with time — see Fig. 7.. | The ratio of small to large-scale magnetic field remains small, and decreases with time – see Fig. \ref{rat}. |
In order to construct realistic synthetic polarization maps it is necessary to complete the simulated magnetic field by addition of an artificial turbulent contribution. | In order to construct realistic synthetic polarization maps it is necessary to complete the simulated magnetic field by addition of an artificial turbulent contribution. |
This is discussed in Sect. 4.. | This is discussed in Sect. \ref{sec:simul}. |
An important result is that by the galaxy age GGyr (Figs. | An important result is that by the galaxy age $T=0.78$ Gyr (Figs. |
3 and 4)), a field of strength B., with a scale of several kpc is already present. | \ref{fig:model138} and \ref{fig:model135}) ), a field of strength $B_{\rm eq}$ with a scale of several kpc is already present. |
This is a more-or-less inevitable result of the initially strong small-scale fields being stretched by differential rotation and then organized by the large-scale dynamo. | This is a more-or-less inevitable result of the initially strong small-scale fields being stretched by differential rotation and then organized by the large-scale dynamo. |
We did also make cursory investigation of the effect of changes in R,. | We did also make a cursory investigation of the effect of changes in $R_\alpha$. |
Specifically,a we looked at cases with Bij=1, with Κω= 10, Ry=2 and Κω=20, Ry=0.5, i.e. the cases shown in Figs. | Specifically, we looked at cases with $B_{\rm inj}=1$, with $R_\omega=10$ , $R_\alpha=2$ and $R_\omega=20$, $R_\alpha=0.5$, i.e. the cases shown in Figs. |
3 and 4 with increased/decreased Ra, respectively. | \ref{fig:model138} and \ref{fig:model135} with increased/decreased $R_\alpha$, respectively. |
The magnetic field geometry is less sensitive to this parameter, and the effect of these changes on field geometry is minor. | The magnetic field geometry is less sensitive to this parameter, and the effect of these changes on field geometry is minor. |
Increasing Κα in the first case increases the regularity of the field at T217 13.2 GGyr (t= 17), and removes any local reversals present. | Increasing $R_\alpha$ in the first case increases the regularity of the field at $T=$ $13.2$ Gyr $t=17$ ), and removes any local reversals present. |
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