deletions | additions       diff --git a/section_Segue_to_RGs_maybe__.tex b/section_Segue_to_RGs_maybe__.tex  index 2ac2218..10142b1 100644  --- a/section_Segue_to_RGs_maybe__.tex  +++ b/section_Segue_to_RGs_maybe__.tex 
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\section{}  %[Segue to RGs: maybe something about the unknown evolution of fields as  %stars evolve]  Both low- and intermediate-mass stars evolve to become red giants when their   hydrogen-core burning is exhausted, leaving a core of helium surrounded by a thin   hydrogen-burning shell, and a thick outer convective envelope.  
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%of maximum power' shows tight correlation with stellar surface gravity[REF  %Brown]].   The comb structure of the spectrum arises from a series of   overtone modes separated by the so-called large frequency separation separation, \dnu. One of these overtone sequences is seen  for each spherical degree, $\ell$. For observations of unresolved distant stars, geometric cancellation prevents detection of modes with $\ell>3$.   Their spectra are therefore dominated characterised  by a pattern of radial ($\ell=0$) and quadrupole ($\ell=2$) modes that form close pairs for each overtone pairs, interspersed  with dipole ($\ell=1$) modes located roughly halfway between successive radial-quadrupole pairs,  with only a weak signal of pairs.  The  octupole modes ($\ell=3$). ($\ell=3$) are weak or undetectable.  %Due to geometric cancellation for higher degree modes, only a weak signal  %of octapole modes are seen and no significant signal for $l>3$.   %[SHORT VERISON: The spectral comb structure arise from a series of  
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\citep{Bedding_2011,Stello_2013,Mosser_2014}  %[REF Bedding2011/Stello2013/Mosser2014]   and to measure radial differential rotation \citep{Beck_2011,Mosser_2012}.   This fortune usefulness  arises because %[through resonance coupling where] each acoustic non-radial modes in the  envelopemode  couples to multiple gravity modes in the core, forming several observable mixed modes %observable at the surface,  with frequencies in the vicinity of the acoustic mode \citep{Beck_2011}.  This coupling is strongest for dipole modes, making them the most useful