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Nitrogen abundance dillerences between the two GC systems was the one piece of evidence that could not be explained in that scenario. | Nitrogen abundance differences between the two GC systems was the one piece of evidence that could not be explained in that scenario. |
We hope that the task of devising a mechanism for the formation of the haloes of the Milkv. Wav and. Andromeda galaxies is made easier bv the findings presented in this paper. | We hope that the task of devising a mechanism for the formation of the haloes of the Milky Way and Andromeda galaxies is made easier by the findings presented in this paper. |
In a forthcoming paper. we contrast measurements of the abundance patterns of M 31 and Galactic GCs. and diseuss their implications to our understanding of the formation of the two galaxy haloes. | In a forthcoming paper, we contrast measurements of the abundance patterns of M 31 and Galactic GCs, and discuss their implications to our understanding of the formation of the two galaxy haloes. |
We thank Sandy Faber for her insightful comments on an early version of this manuscript aud Jay Strader for inspiring discussions. | We thank Sandy Faber for her insightful comments on an early version of this manuscript and Jay Strader for inspiring discussions. |
We also acknowledge the fundamental contribution made by Jim Rose at the early stages of this project. | We also acknowledge the fundamental contribution made by Jim Rose at the early stages of this project. |
An anonvmots releree is thanked. lor useful suggestions deriving [rom a careful and thorough readiug of the original manuscript. | An anonymous referee is thanked for useful suggestions deriving from a careful and thorough reading of the original manuscript. |
RPS appreciatles the support from Gemini Observatory. which is operated bv the Association of Universities for Research in Astronomy. Ine.. on behalf of ihe international Gemini partnership of Argentina. Australia. Brazil. Canada. Chile. the United Ixingdom. and the United States of America. | RPS appreciates the support from Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the United Kingdom, and the United States of America. |
The hospitality of the Department of Astrophysical Sciences at Princeton University. where this paper was partly conceived. is warmnlv acknowledged. | The hospitality of the Department of Astrophysical Sciences at Princeton University, where this paper was partly conceived, is warmly acknowledged. |
S.C. acknowledges (he support through a Discovery Grant [rom the Natural Sciences and Engineering Research Council of Canada. | S.C. acknowledges the support through a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada. |
(Iirosawa2006).. reaching magnitude V—4.5 at this time. | \citep{hir06}, reaching magnitude V=4.5 at this time. |
For the purposes of this paper. we deline this as /=0. | For the purposes of this paper, we define this as $t = 0$. |
The optical light curve then began a rapid decline. very. similar to (hat seen in previous outbursts (IRosino1987.. AAVSO!)). | The optical light curve then began a rapid decline, very similar to that seen in previous outbursts \citealt{ros87}, ). |
Several lines of evidence are consistent wilh a distance to RS Oph of 1.6z0.3 kpe (Bode1987). | Several lines of evidence are consistent with a distance to RS Oph of $1.6\pm0.3$ kpc \citep{bod87}. |
. The RS Oph binary svstem comprises a red eint star in a 455.72z0.83 dav orbit. with a white dwarl (WD) of mass near the Chandrasekhar limit (seeDobrzvcka&Ixenvon1994:Shoreοἱal.1996:Fekel 2000). | The RS Oph binary system comprises a red giant star in a $455.72\pm0.83$ day orbit with a white dwarf (WD) of mass near the Chandrasekhar limit \citep[see][]{dob94,sho96,fek00}. |
. Accretion of hvdrogen-rich material from the red giant onto the WD surface leads to the conditions for a thermonuclear runaway (TNR) in a similar fashion to that for classical novae (CNe). | Accretion of hydrogen-rich material from the red giant onto the WD surface leads to the conditions for a thermonuclear runaway (TNR) in a similar fashion to that for classical novae (CNe). |
The much shorter inter-outburst. period for this tvpe of RN compared to CNe is thought to be due to a combination of the high WD mass aud a supposed high accretion rate (e.g.Sturlieldetal.1935:Yaron2005). | The much shorter inter-outburst period for this type of RN compared to CNe is thought to be due to a combination of the high WD mass and a supposed high accretion rate \citep[e.g.][]{sta85,yar05}. |
. Such models lead to the ejection of somewhat lower masses at higher velocities than those for models of CN (typically 5000 km | and 10/7—10 SAL. respectively for Rove), | Such models lead to the ejection of somewhat lower masses at higher velocities than those for models of CN (typically 5000 km $^{-1}$ and $10^{-8} - 10^{-6}$ $_\odot$ respectively for RNe). |
Spectroscopy of RS Oph has indeed shown Ila line emission with FWIIM =3930 kms ! and FWZI =7540 km Lon 2006 February 14.2 (=1.37 davs. Duil2006)). | Spectroscopy of RS Oph has indeed shown $\alpha$ line emission with FWHM $= 3930$ km $^{-1}$ and FWZI $= 7540$ km $^{-1}$ on 2006 February 14.2 $t = 1.37$ days, \citealt{bui06}) ). |
Unlike CNe. where the mass donor is a low-mass main-sequence star. the presence of the red giant in the RS Oph svstem means that the high velocity ejecta run into a dense circumstellar medium in (he form of (he red giant. wind. setting up a shock svstem with gas temperattres ~2.2x LOIN for ος=4000 kms |. where vy is the velocity of the forward shock running into the pre-existing wind. | Unlike CNe, where the mass donor is a low-mass main-sequence star, the presence of the red giant in the RS Oph system means that the high velocity ejecta run into a dense circumstellar medium in the form of the red giant wind, setting up a shock system with gas temperatures $\sim 2.2 \times 10^{8}$ K for $v_{S} = 4000$ km $^{-1}$ , where $v_S$ is the velocity of the forward shock running into the pre-existing wind. |
X-rav observations of the 2006 outburst by and Sokoloskietal.(2006) have confirmed the basic shock model of and O'Brienetal.(1992) in which RS Oph evolves like a supernova remnant (SNR). but on timescales around. 107? times Laster. | X-ray observations of the 2006 outburst by \cite{bod06} and \cite{sok06} have confirmed the basic shock model of \cite{bod85} and \cite{obr92} in which RS Oph evolves like a supernova remnant (SNR), but on timescales around $10^5$ times faster. |
VLBI imaging at Gem ancl L&em began 13.8 days after outburst (O'Brienetal.2006). | VLBI imaging at 6cm and 18cm began 13.8 days after outburst \citep{obr06}. |
. The initial image showed a partial ring of non-thermal (synchrotron) emission. of radius 13.8 AU at d=1.6 kpe. consistent with emission from the forward shock. | The initial image showed a partial ring of non-thermal (synchrotron) emission, of radius 13.8 AU at $d = 1.6$ kpc, consistent with emission from the forward shock. |
Subsequently. more extended lobes aligned E-W exadually emerged. with that in the East appearing first. | Subsequently, more extended lobes aligned E-W gradually emerged, with that in the East appearing first. |
This morphology was consistent with that derived from more rudimentary VLBI observations 77 davs after the 1985 outburst by Tayloretal.(1989).. apparently showing jets of emission. | This morphology was consistent with that derived from more rudimentary VLBI observations 77 days after the 1985 outburst by \cite{tay89}, apparently showing jets of emission. |
O'Brienetal.(2006) proposed a simple geometrical model comprising an expanding lobed structure. wilh the major axis perpendicular to the proposed plane of (he central binary orbit. | \cite{obr06} proposed a simple geometrical model comprising an expanding double-lobed structure, with the major axis perpendicular to the proposed plane of the central binary orbit. |
llere we report IIubble Space Telescope (7/97) observations of the expanding nebular remnant taken al /= 155dand compare them to the structures seen earlier in (he radio. | Here we report Hubble Space Telescope ) observations of the expanding nebular remnant taken at $t = 155$ dand compare them to the structures seen earlier in the radio. |
We | We |
The slow rotation rates of low to intermediate mass C 2A.) preanaimn-sequeuce stars remains one of the nost portant aspects of star formation that has. so far. resisted a ecuerally accepted explanation. | The slow rotation rates of low to intermediate mass $\la 2 M_\odot$ ) pre-main-sequence stars remains one of the most important aspects of star formation that has, so far, resisted a generally accepted explanation. |
By the time hey become optically visible as T Tauri stars1915).. approximately half thei are observed to rotate at approximately of breakupof speed2007). | By the time they become optically visible as T Tauri stars, approximately half of them are observed to rotate at approximately of breakup speed. |
. This is a surprise because παν TTSs1: Classical T Tauri stars: CTTSs) ire actively accreting material from surrounding Keplerian disks2001). | This is a surprise because many TTSs (the Classical T Tauri stars; CTTSs) are actively accreting material from surrounding Keplerian disks. |
. At a typical accretion rate of AL,~10SAR wrtf. the angular momentiun deposited by accreting disk material should spin up a CTTS to uear breakup speed in ~109 vears2007). | At a typical accretion rate of $\dot M_{\rm a} \sim 10^{-8} M_\odot$ $^{-1}$, the angular momentum deposited by accreting disk material should spin up a CTTS to near breakup speed in $\sim 10^6$ years. |
. Since the acerction pliase lasts for 10° LOT years2006).. since the stars acerete at auch higher rates prior to the TTS phase. and since the stars are still contracting102).. an cficient angular momentum loss mechanisin is required to explain the existence of the slow rotators. | Since the accretion phase lasts for $10^6$ – $10^7$ years, since the stars accrete at much higher rates prior to the TTS phase, and since the stars are still contracting, an efficient angular momentum loss mechanism is required to explain the existence of the slow rotators. |
A few interesting aud important ideas for explaining the TTS slow rotators have been developed over the last two decades. | A few interesting and important ideas for explaining the TTS slow rotators have been developed over the last two decades. |
These have resulted in the "star-disk interaction model of1978). applied to CTTSs bvuiel91. the N-wind model1991).. aud the idea that stellar winds provide strong torques2005a). | These have resulted in the star-disk interaction model of, applied to CTTSs by, the X-wind model, and the idea that stellar winds provide strong torques. |
. Although both have advanced our understanding of the magnetic star-disk interaction. neither the Cohosh Lainh nor N-wiud models are without problems2005)h).. and the idea that stellar winds are mnaportaut has not vet been worked out in sufficient detail to compare to he other models. | Although both have advanced our understanding of the magnetic star-disk interaction, neither the Ghosh Lamb nor X-wind models are without problems, and the idea that stellar winds are important has not yet been worked out in sufficient detail to compare to the other models. |
TnD.. we tuther explored powerful stellar winds as a solution o the angular momentum problem and suggested. that a fraction of the accretion power provides the energv recessary to drive the wind. | In, we further explored powerful stellar winds as a solution to the angular momentum problem and suggested that a fraction of the accretion power provides the energy necessary to drive the wind. |
We showed that stellar winds are capable of carrvine off the accreted augular uonientun. provided tha EAMAL,~O.1. where EAM is the outflow rate of maeral that is magnetically connected to the star {the "stellary. wind”). | We showed that stellar winds are capable of carrying off the accreted angular momentum, provided that $\dot M_{\rm w} / \dot M_{\rm a} \sim 0.1$, where $\dot M_{\rm w}$ is the outflow rate of material that is magnetically connected to the star (the “stellar wind”). |
This analysis included a formulation for the stellar wind torque that contained the Alfvémn radius (r4). which is not easily deteriuued a priori iu the wind. and the conclusions were based on a one-dimensional scaling estinate of this miportaut physical quautitv. | This analysis included a formulation for the stellar wind torque that contained the Alfvénn radius $r_{\rm
A}$ ), which is not easily determined a priori in the wind, and the conclusions were based on a one-dimensional scaling estimate of this important physical quantity. |
Thus. while it is clear that aceretion-powered stellar: winds (APSWs) can in principle provide the necessary spin-down torque. this idea requires further development to produce a more detailed model. | Thus, while it is clear that accretion-powered stellar winds (APSWs) can in principle provide the necessary spin-down torque, this idea requires further development to produce a more detailed model. |
Toward this goal. used 2-dimensional (axisviunetiic) maegnetohydrodvuanuc— simulations to solve for ry aud caleulate realistic stellar wind torques for a range of paralucters. | Toward this goal, used 2-dimensional (axisymmetric) magnetohydrodynamic simulations to solve for $r_{\rm A}$ and calculate realistic stellar wind torques for a range of parameters. |
In the preseut paper. we use the stellar wind solutions of Paper II to compare the stellar wiud torque to the torques expected to arise from the star-disk iuteraction. | In the present paper, we use the stellar wind solutions of Paper II to compare the stellar wind torque to the torques expected to arise from the star-disk interaction. |
Furthermore. we fud new solutions for stellar spins. based upon torque balance between the accretion torque and the APSW spin-down torque. | Furthermore, we find new solutions for stellar spins, based upon torque balance between the accretion torque and the APSW spin-down torque. |
This paper beeius with a brief description of the simulation | This paper begins with a brief description of the simulation |
condition (i) Caen requires that e>0. e>0. and b>—(dac)! | condition (iii) then requires that $a>0$ , $c>0$ , and $b>-(4ac)^{1/2}$. |
With this form for g(s). there is an unstable region (g'(s)<0) if and only if 7, | With this form for $g(s)$, there is an unstable region $g'(s)<0$ ) if and only if $b<-(3ac)^{1/2}$ . |
When this condition is satisfied. all values of is) between s,>0 and sj>0 are unstable. whereESTEDi The interval s,<[s|&sj in which a uniform shear is unstable is called the spinodal interval (Figure 1)). | When this condition is satisfied, all values of $|s|$ between $s_a>0$ and $s_b>0$ are unstable, where; The interval $s_a<|s|<s_b$ in which a uniform shear is unstable is called the spinodal interval (Figure \ref{fig:ggg}) ). |
There is also interesting behavior outside (he spinodal interval. | There is also interesting behavior outside the spinodal interval. |
Suppose that the svstem is in uniform shear sj outside the spinodal interval. ο>ορ. | Suppose that the system is in uniform shear $s_1$ outside the spinodal interval, $s_1>s_b$. |
Suppose that there is another shear state outside the spinodal interval. so« s,. such that g(s4)=g(se). | Suppose that there is another shear state outside the spinodal interval, $s_2<s_a$ such that $g(s_1)=g(s_2)$. |
Then if a small element 0.7 changes ils shear state [rom s( (0 s». and the remaining fhuid increases its shear rate [rom s, to sy+05, 80 as (o satis[v the mean shear constraint (5)). the resulting change in [ree energy 15 or[G(sa)—G(s.)G(s,)(s254)]. which is negative if | Then if a small element $\delta x$ changes its shear state from $s_1$ to $s_2$ , and the remaining fluid increases its shear rate from $s_1$ to $s_1+\delta s_1$ so as to satisfy the mean shear constraint \ref{eq:bc}) ), the resulting change in free energy is x[G(s_2)-G(s_1)-G'(s_1)(s_2-s_1)], which is negative if G'(s_1)=g(s_1)>. |
Shear states in which this inequality is satisfiedthe intervals,€s«s; ands,<s<5, in Figure l- ave metastable. because the mixture of two distinct phases has a lower [ree energy. | Shear states in which this inequality is satisfied—the interval $s_p<s<s_a$ and $s_b<s<s_q$ in Figure \ref{fig:ggg}- —are metastable, because the mixture of two distinct phases has a lower free energy. |
Equation (20)) is ill-posed. since (he growth rate of the instability(5)) becomes extremely largee for short-wavelengthe disturbances. | Equation \ref{eq:ch}) ) is ill-posed, since the growth rate of the instability\ref{eq:instab})) becomes extremely large for short-wavelength disturbances. |
It is convenient. and physically plausible.to mitigatee (his violent instability bymocdifving equation (20)) to a | It is convenient, and physically plausible,to mitigate this violent instability bymodifying equation \ref{eq:ch}) ) to , |
It is convenient. and physically plausible.to mitigatee (his violent instability bymocdifving equation (20)) to a: | It is convenient, and physically plausible,to mitigate this violent instability bymodifying equation \ref{eq:ch}) ) to , |
Tere. we describe a next generation x-rav fiume mission which would offer au order of maguitude increase in x-ray timing capabilities via an x-ray detector witli a geonietie area of at least 60.000 ο”, equal to ten times that of RNTE. | Here, we describe a next generation x-ray timing mission which would offer an order of magnitude increase in x-ray timing capabilities via an x-ray detector with a geometric area of at least 60,000 $^2$, equal to ten times that of RXTE. |
The most inportant advances made with this order of magnitude increase m collecting area are likely to be true discoveries and thus camnot be anticipated. | The most important advances made with this order of magnitude increase in collecting area are likely to be true discoveries and thus cannot be anticipated. |
However. au order of inagnitude increase in area would benefit may scientific investigations. | However, an order of magnitude increase in area would benefit many scientific investigations. |
Here. we describe three particular examples. ( | Here, we describe three particular examples. ( |
BICs) have been discovered in three systems with frequencies of 67-300 Tz (Remillard et al. | BHCs) have been discovered in three systems with frequencies of 67-300 Hz (Remillard et al. |
1999). | 1999). |
The fast OPOs from BIICs are rather weak (uus amplitudes near 1%)} aud difficult to study in detail with RNTE. | The fast QPOs from BHCs are rather weak (rms amplitudes near ) and difficult to study in detail with RXTE. |
A umuber of models of the QPOs have been proposed. all of which involve strone-field general relativistic effects. but distinguishing amougst the various models will be difficult with the RNTE data. | A number of models of the QPOs have been proposed, all of which involve strong-field general relativistic effects, but distinguishing amongst the various models will be difficult with the RXTE data. |
The increase in the photon statistics with RAE would make possible much more accurate measurements of the QPO paramcters aud their variatious with time or correlations with spectral or other timing parameters. | The increase in the photon statistics with RAE would make possible much more accurate measurements of the QPO parameters and their variations with time or correlations with spectral or other timing parameters. |
This may lead to a uuique identification of the ΟΡΟ ecueration mechanism. | This may lead to a unique identification of the QPO generation mechanism. |
Vuderstanding these QPOs would provide a unique probe of strong-ficld gravity. | Understanding these QPOs would provide a unique probe of strong-field gravity. |
have beendiscovered from a uber of neutron stars. | have been discovered from a number of neutron stars. |
The oscillations have periods in the ranee 1.7-9 nis and are interpreted as due to inhomogeneous nuclear buruine of matter initially located ou the neutron star surface. | The oscillations have periods in the range 1.7-3 ms and are interpreted as due to inhomogeneous nuclear burning of matter initially located on the neutron star surface. |
The burst oscillations provide a means to constrain the jeutron star mass-racdius relation. | The burst oscillations provide a means to constrain the neutron star mass-radius relation. |
Currently. the best coustraiut comes from a deep nodulation (το+ 17%) ποσα in the initial 62.5 ius of oue burst (Strolumaver ct al. | Currently, the best constraint comes from a deep modulation $75\% \pm 17\%$ ) seen in the initial 62.5 ms of one burst (Strohmayer et al. |
L998). | 1998). |
RAE would detect roughly 1000 counts in each oscillation cevele near the »ea of a typical bright burst. | RAE would detect roughly 1000 counts in each oscillation cycle near the peak of a typical bright burst. |
This would permit detailed examination of individual oscillation cycles and allow accurate measurement of the modulation amplitude iu he first few oscillation cycles. | This would permit detailed examination of individual oscillation cycles and allow accurate measurement of the modulation amplitude in the first few oscillation cycles. |
Both our uuderstaudiug of the burst oscillations aid constraints on the neutron star niass-radius relation would iuprove. | Both our understanding of the burst oscillations and constraints on the neutron star mass-radius relation would improve. |
of the accreting maguctic white dwart NY Arietis showed that he x-ray flux einerges from eclipse egress in «2 s (eller 1997). | of the accreting magnetic white dwarf XY Arietis showed that the x-ray flux emerges from eclipse egress in $< 2$ s (Hellier 1997). |
For the previous 15 vears. the fraction. f. of the white dwarf surface involved in x-ray clussion lacl )en debated with values raneing from 0.001 to 0.3. | For the previous 15 years, the fraction, $f$, of the white dwarf surface involved in x-ray emission had been debated with values ranging from 0.001 to 0.3. |
Ποιαs result. obtained by combining 20 RATE observations. shows that f«0.002. | Hellier's result, obtained by combining 20 RXTE observations, shows that $f < 0.002$. |
Using RAE. au accurate estimate could be made of the emittiug region location on each egress which would allow direct mapping of movement of the cutting region. | Using RAE, an accurate estimate could be made of the emitting region location on each egress which would allow direct mapping of movement of the emitting region. |
Similar mapping cau also be done in neutron star and black hole binaries. | Similar mapping can also be done in neutron star and black hole binaries. |
The best coustraiunts currently available on the size of the x-ray. euüttiug regions m black hole svstenis come from x-ray dips (e.g. Tomsick et al. | The best constraints currently available on the size of the x-ray emitting regions in black hole systems come from x-ray dips (e.g. Tomsick et al. |
1997). | 1997). |
RAE would lead to significant advances iu mapping x-ray Cluission from many different x-ray sources. | RAE would lead to significant advances in mapping x-ray emission from many different x-ray sources. |
The Relativistic Astrophysics Explorer (RAE) will consist of two scicutific instruments: a large area x-ray detector and a wide-field x-ray monitor. | The Relativistic Astrophysics Explorer (RAE) will consist of two scientific instruments: a large area x-ray detector and a wide-field x-ray monitor. |
RAE will be designed to have telemetry sufficient to transimit the large event rate aud flexible operations | RAE will be designed to have telemetry sufficient to transmit the large event rate and flexible operations |
Theeiiploxiueut of stellar temperatures from spectroscopiulch. aalvsis of iron Imes iuscad ofpublished colours avoids the use of uncertain recdening estimations. | The employment of stellar temperatures from spectroscopic analysis of iron lines instead of published colours avoids the use of uncertain reddening estimations. |
The results of the revlewed analysis of the old sample xd of the analysis of the new sample. published iu Paceal.(2009)... were usec to produce the diagram of CA as a function of temperature shown in Figure I.. | The results of the reviewed analysis of the old sample and of the analysis of the new sample, published in \cite{letter}, were used to produce the diagram of CA as a function of temperature shown in Figure \ref{fig}. |
Tt was already pointed «mt back in the cightics that the distribution of CA is markedly bimodal (VanenuiPreston 1980). | It was already pointed out back in the eighties that the distribution of CA is markedly bimodal \citep{vpgap}. |
Niuncehs 7overv few stars are less active than the παςος aud siguificautlv nore active than the Sun. | Namely very few stars are less active than the Hyades and significantly more active than the Sun. |
This 1uderpopulated range of values is usualv referred to as VaughanPreston (VP) gap. | This underpopulated range of values is usually referred to as Vaughan–Preston (VP) gap. |
armom(al.(1981) explained it as a coubiued effect of CA saturation 1j active stars and a basal level in twe CA indicator used bv VP. due to the plotospleric fix. | \cite{hartmann} explained it as a combined effect of CA saturation in active stars and a basal level in the CA indicator used by VP, due to the photospheric flux. |
These. it was claiuect. enhance the nmuüpression of a eap. | These, it was claimed, enhance the impression of a gap. |
A variation in the local stellar birthrate was also vosed. | A variation in the local stellar birthrate was also invoked. |
Other studies consider the VP. eap a result of the nature of the CA evolution (c.g.Durneyctal.1981:Middelkoop. | Other studies consider the VP gap a result of the nature of the CA evolution \citep[e.g.][]{dmr81,
middelk}. |
1982 ).. Our Figure 1 corroborates the atter hvpothesis: all stars vounecr than 1.2 Ch. exeeot oue. lie above the eap. all stars older than 1.1 Cyr with the exceptiou of one. lie below it. iudicatiug a drop of CA level in a very short time. | Our Figure \ref{fig} corroborates the latter hypothesis: all stars younger than 1.2 Gyr, except one, lie above the gap, all stars older than 1.4 Gyr with the exception of one, lie below it, indicating a drop of CA level in a very short time. |
The two CXCÓions are probably due to a particular phase of he activity cycle. | The two exceptions are probably due to a particular phase of the activity cycle. |
It is worth noticing that the stars in either side of he eap differ not oulv in CA level. mit also iu its trend as a function of teniperature: og.y/ (or. equivaleutlyMe- log./ Ripe) depeuds. weakly-d.e ou he temperature or stars above the gap. while it has a distiact decreasing trend for stars below. | It is worth noticing that the stars in either side of the gap differ not only in CA level, but also in its trend as a function of temperature: $\log R^{\prime}_K$ (or equivalently $\log
R^{\prime}_{HK}$ ) depends weakly on the temperature for stars above the gap, while it has a distinct decreasing trend for stars below. |
This can )6 seen from our Fieure 1.. and itappears clearer when a larger tenipeorature raice is considered. like. OY Musance. 1ji Mamajek&Illeubraud (2008.. sec Figure L therein). | This can be seen from our Figure \ref{fig}, and itappears clearer when a larger temperature range is considered, like, for instance, in \citeauthor{MH} \citeyear{MH}, see Figure 4 therein). |
Furtheriuore. shortterm temporal variatious of CA are laree aid inreeular for active stars and simal and regular for inactive ones (Vaughan 19803. | Furthermore, short–term temporal variations of CA are large and irregular for active stars and small and regular for inactive ones \citep{cycles}. |
. There uust be a major event at a eiven time of the stellar aad ποποιος ifo time. that chanecs the wav radiaive heating mechanisius occur iu the chromosphere. ancl. as a consequence. their depeideuce ou stellar paraucters as well as the shape aud leugth of CA cveles. | There must be a major event at a given time of the stellar main sequence life time, that changes the way radiative heating mechanisms occur in the chromosphere, and, as a consequence, their dependence on stellar parameters as well as the shape and length of CA cycles. |
Fawzyctal.(2002) present theoretical calcuations that reproduce the observed trend of CA with stellar temperature. | \cite{fawzy} present theoretical calculations that reproduce the observed trend of CA with stellar temperature. |
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