Solar Ellerman Bombs in 1-D Radiative Hydrodynamics

0.21 MB·

by  A. Reid

DraftversionJanuary17,2017
PreprinttypesetusingLATEXstyleemulateapjv.5/2/11
SOLARELLERMANBOMBSIN1-DRADIATIVEHYDRODYNAMICS
A.Reid1,4,M.Mathioudakis1,A.Kowalski2,3,J.G.Doyle4,J.C.Allred5
1.AstrophysicsResearchCentre,SchoolofMathematicsandPhysics,Queen’sUniversityBelfast,BT71NN,NorthernIreland,UK;e-mail:
[email protected]
2.DepartmentofAstrophysicalandPlanetarySciences,UniversityofColoradoBoulder,2000ColoradoAve,Boulder,CO80305,USA.
3.NationalSolarObservatory,UniversityofColoradoBoulder,3665DiscoveryDrive,Boulder,CO80303,USA
4.ArmaghObservatoryandPlanetarium,CollegeHill,Armagh,BT619DG,UK
5.NASA/GoddardSpaceFlightCenter,Code671,Greenbelt,MD20771
7
1 DraftversionJanuary17,2017
0
2 ABSTRACT

n Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive
a brighteningsinhightemperaturelines,whichwhencombinedwithsimultaneousgroundbasedobservationsin
J Hα, appear co-spatialto Ellerman Bombs(EBs). We use the RADYN 1-dimensionalradiativetransfer code

6 inanattempttotryandreproducetheobservedlineprofilesandsimulatetheatmosphericconditionsofthese
1 events.CombinedwiththeMULTI/RHlinesynthesiscodes,wecomputetheHα,CaII8542Å,andMgIIh&
klinesforthesesimulatedeventsandcomparethemtopreviousobservations. Ourfindingshintthatthepres-

] enceofsuperheatedregionsinthephotosphere(>10,000K)isnotaplausibleexplanationfortheproduction
R
ofEBsignatures.WhileweareabletorecreateEB-likelineprofilesinHα,CaII8542Å,andMgIIh&k,we
S
cannotachieveagreementwithallofthesesimultaneously.
.
h Subjectheadings:Sun:Activity—Hydrodynamics—Sun:Photosphere
p
-
o
1. INTRODUCTION versionsof these events show evidence for flux cancellation
r
t Ellerman Bombs (EBs henceforth) were first noticed in (Reidetal.2016),withmagneticenergiescomparabletothat
s
of the radiative energy losses. EBs have been estimated
a Ellerman (1917), who noted brightenings in the wings of
[ the Hα, Hβ, and Hγ lines. These events have also been to form in the temperature minimum region (Nelsonetal.
2015), with foot-points reported to form as low as 300 km
observed in the wings of Ca II 8542 Å (Fangetal. 2006;
1 (Watanabeetal.2011). As such, they are thoughtto appear
v Socas-Navarroetal. 2006; Pariatetal. 2007; Vissersetal. duetophotosphericmagneticreconnection,occurringaround
3 2015; Lietal. 2015), as well as in Ca II H images thetemperatureminimumregion,wherethisprocessismost
1 (Matsumotoetal.2008a;Hashimotoetal.2010). Theyshow efficient(Litvinenko 1999).
2 noobservableenhancementinthecoreoftheselineprofilesas
Three-dimensionalnumericalmodelingofphotosphericre-
4 theseareformedintheoverlyingchromosphericcanopy.EBs
connectionhasshownlocaltemperatureincreasesinthepho-
0 are considered a solely photospheric/lower chromospheric
tosphere by a factor of 1.1-1.5 relative to quiet Sun, along
. phenomenon(Vissersetal.2013).
1 withadensityincreasebyafactorof4atthemagneticinver-
EBbrighteningsarealsoobservableintheSolarDynamics
0 sionline(Archontis&Hood 2009). TheArchontis&Hood
7 Observatory(SDO) 1700Å and 1600Å channels(Qiuetal. (2009) model has also shown bi-directional flows in the re-
1 2000;Georgoulisetal.2002;Pariatetal.2007;Berlickietal. gion, with values of 2-4 km s−1. Semi-empirical models
: 2010; Vissersetal. 2013), though to a lesser degree than for EBs show localized temperature enhancements of 600-
v
the Hα line wings due to the broad passbands of these
i 3000K aroundthe temperatureminimumregion(Fangetal.
X filters encompassing a wide range of atmospheric heights 2006; Berlicki&Heinzel 2014). These temperature en-
r (Vissersetal.2013). While the 1600 Å channel offers bet- hancements lead to intensity enhancements in the wings of
a ter contrast than the 1700 Å channel (Ruttenetal. 2013; the Hα and Ca II 8542 Å lines. Other EB studies also find
Vissersetal.2013), EB signatures are more difficult to ob- similartemperatureenhancements(200-3000K)inthephoto-
serveinthe1600Åchannelduetocontaminationeffectsfrom sphere/temperatureminimumregion(Georgoulisetal.2002;
CIVemissionwithtransitionregiontemperatures. Isobeetal.2007;Yangetal.2013;Hongetal.2014;Lietal.
EBs typically last for a few minutes, and appear rather 2015).
impulsivelyincomparisonwithotherphotosphericbrighten- EBs have also been foundwithin quiet Sun regionsof the
ings such as moving magnetic features (MMFs). Reidetal. photosphere (Rouppevandervoortetal.2016). The obser-
(2016) have shown that by introducing an impulsivity crite- vationalsignaturesoftheseQSEBsarenotaspronouncedas
rion, it is possible to distinguish between pseudo-EBs and thosefoundinthevicinityofactiveregions,thoughtheyare
EBs. EBs aregenerallyobservedwith co-spatialblue-shifts, stilllocatedinregionsofoppositepolaritymagneticflux.This
or bi-directional Doppler shifts (Matsumotoetal. 2008a; suggeststhattheseeventsareidenticaltoEBsoccurringatlo-
Watanabeetal.2011). cationsofweakermagneticfluxcancellation.
EBs are generally found in regions of opposite polarity More recently, observations using the IRIS instrument in-
magnetic flux (Georgoulisetal.2002; Watanabeetal.2008; dicate that EB signatures have been foundin the Mg II h &
Matsumotoetal.2008b;Hashimotoetal.2010;Nelsonetal. k wings, Si IV, and C II lines (Peteretal.2014; Kimetal.
2013; Vissersetal. 2013). Recent spectropolarimetric in- 2015; Vissersetal.2015; Tianetal.2016). These lines are
2 Reidetal.
Figure1. TopLeft:SynthesisedHαlineprofilesforenergiesdepositedatvariousheights,usingthequietSunstartingatmosphere.TopRight:Thecorresponding
CaII8542Ålineprofiles.BottomLeft:Temperatureprofilesacrossthetemperatureminimumregion.BottomCenter:Verticalvelocityprofiles.BottomRight:
Electrondensityprofiles.
sensitivetomuchhighertemperatures(50,000-100,000K), 8542Å,andMgIIh&klineprofilestocomparewithobser-
and sample the upper chromosphere and transition region. vations. Thecodealsohastheabilitytoapplyatimedepen-
Vissersetal.(2015) suggest that they are formed below the dent heating function into the atmosphere, and thus is aptly
chromosphericcanopyduetosuperheatingwithtemperatures suitedforthestudyofEBs.
upto80,000K.Judge (2015)hasdebatedtheoriginsofthese Our RADYN simulationsuse the quietSun starting atmo-
bombsonthebasisthattheUVphotonsdetectedintheSiIV sphere(QS.SL.LTinAllredetal.(2015)). Atimedependent
linecannotescapeifformedbelow500kmabovethephoto- heatingfunctionisappliedto theatmosphere,allowingfora
sphericfloor. rangeofenergydepositionratesovervariousportionsofthe
The MURaM code used by Reidetal.(2015) shows Hα photosphere/lowerchromosphere. TheMULTIlinesynthesis
wing enhancement at the magnetic inversion line of a bipo- code is used to synthesise the Hα and Ca II 8542Å lines to
larstructure,co-spatialwithtemperatureenhancements.This attempt to replicate the signatures of the observed line pro-
eventhasshownfluxcancellation,thoughthesimulationwas fileswithemissioninthewings,whileleavingthelinecores
ofquietSun,andsowasmorelikelyaQSEB.Withthestrong unchanged.
variance in temperatures required to produce the EB signa- PreviousestimatesofEBenergiesareinthe rangeof1024
tures, synthesising these line profiles from hydrodynamical -1027 ergs(Georgoulisetal.2002;Fangetal.2006;Lietal.
simulations can help clarify the processes involved and also 2015; Reidetal.2016). If we assume a lifetime of ∼5 min-
offersanalternativeapproachtoEBlineformationmodeling. utes,andanactivereconnectionareaof300km2, theenergy
Inthisstudy,weusetheRADYNcodetomodelanEB-like deposition rate would need to be of the order of 100 - 1000
atmosphere,withcorrespondingsynthesisoftheHα(Section ergs/cm3/sec,assumingaverticalextentof∼200km.
2),CaII8542Å(Section2),andMgIIh&k(Section3)line A grid of models was set up, applying heating rates be-
profiles for comparison with previous observational studies tweenthesevaluesover200kminthephotosphere(seeGrid
(e.g.Vissersetal.(2015)). 1fromTable1). Theatmospheretakesroughly9secondsto
stabilize after the heating is applied, with all measurements
2. HαANDCAII8542ÅMODELING taken at T=10s. A temperature enhancement appears at the
locationofenergydeposition,rangingbetween300-2600K,
The RADYN code (Carlsson&Stein 1992, 1994, 1995)
with2600Krelatingtothe1000ergs/cm3/secdepositionrate.
has been used extensively to study flare dynamics via beam
This is accompanied by an associated local electron density
heatingina1-dimensionalsolaratmosphere.RubiodaCosta
enhancement. Duetothesuddeninjectionofenergy,ashock
(2016)usedtheRADYNcodeinanattempttomodeltheat-
forms at the deposition location. This creates bi-directional
mosphere of an X1.0 solar flare, synthesising the Hα, Ca II
INVESTIGATINGIRIS/ELLERMANBOMBSIN1-DRADIATIVEHYDRODYNAMICS 3
velocityflowsupto 2kms−1. Theupwardvelocityis atthe energydepositedaroundthetemperatureminimumexponen-
leading edge of the shock and is stronger than the weaker, tially, between1000- 1 x106 ergs/cm3/sec(Grid3). Again,
trailingdownflow. noenhancementisobservedintheMgIIh&klines,though
With the associated synthesised Hα line profiles, it was strong continuum enhancement appears with these high en-
apparent that although the 100 ergs/cm3/sec could create a ergydepositionrates. Theatmosphericresponseto thissud-
smallenhancement,itwasnotsufficienttopushthelinewings denenergeticinjectiondidnotcreatedramaticallyhighertem-
into emission. With energy deposition rates of 300 - 700 peratures.Infact,thepeaktemperatureinthe1x106ergs/cm3
ergs/cm3/sec, the Hαline wingenhancementwas 150%that modelreached9500K,withacorrespondingelectrondensity
of the background profile, while a deposition rate of 1000 of1014cm−3andapeakshockvelocityof5kms−1.
ergs/cm3/sec appeared to more than double the line wing ThecontributionfunctionoftheMgIIh&klinesappeared
emissioninHα,whilealsoenhancingthecontinuumby20%, toshowalinecoreformationheightconcentratedintheupper
whichiscontrarytoobservations. chromosphere,with little contributionfromthephotosphere.
Anenergydepositionrateof500ergs/cm3/secwasthought The wings of the lines were formedslightly lower, closer to
to be sufficient to replicate an EB-like enhancement in the
thelinecoreformationregionofCaII8542Å.Iftheenergy
wingsofHα. Thisenergywastheninjectedover200km,and
depositionoccursin the lower-midchromosphere,enhanced
placedacrossvariousregionsofthephotosphere/temperature
emission in the Mg II h & k wings can be achieved, though
minimumregioninanattempttolocatetheformationheight
thiswillonlycauseflare-likeprofilesproducingfullemission
of EBs (Grid 2). We also modeled the emission in the Ca
inCaII8542ÅandHα(Grid4).
II 8542 A line, because, by consideringtwo lines formed at
It also became apparentthat the backgroundMg II h & k
differentheights, we can better constrain the location of EB
line profile of our model appeared in absorption rather than
energy deposition. Fig. 1 shows the response of the atmo-
in emission as is observed. In an attempt to rectify this is-
sphere to the injected energy, along with the corresponding
sue, a different starting atmosphere was adopted which has
lineprofiles.
it’s transition regionpushedto highercolumn masses, to re-
Sincethedensitydecreaseswithincreasingheight,deposit-
flect a more active, plage-like atmosphere (QS.SL.HT from
ing energy higher in the atmosphere results in greater tem-
(Allredetal.2015)).
peratureenhancements. Amaximumtemperatureof9000K
With this new starting atmosphere, the initial profile of
wasgeneratedinGrid2.Bi-directionalflowsarealsoformed,
withpeakvelocitiesupto5kms−1.Thesevaluesarestronger the Mg II h & k lines appear in emission, similar to the
backgroundprofilesobserved(Peteretal.2014;Vissersetal.
than thatof Grid 1. The electrondensity increase is notlin-
2015; Kimetal.2015; Tianetal.2016). However, the line
ear with the heightof injected energy. The increase appears
toplateauaround1.5x1013cm−3. Thisnon-linearbehaviour coresofCaII8542ÅandHαarealsoslightlyenhanced,with
CaII8542Åbeingmoreprominent.
is also apparent in the corresponding Hα and Ca II 8542 Å
Again, two grids of models were run, one grid applying
lineprofiles,withthegreatestdifferenceinthewingemission
1000ergs/cm3/secofheatingin200kmdepthsoverthepho-
beingatthelowerinjectedheightswithinGrid2. AsmallHα
tosphereandtemperatureminimum,similartoFig.1(Grid5).
coreenhancementisalsoapparentinthesimulations.Thisef-
Thesecondgridappliedthesameheatingfunctioninthechro-
fectcouldbegreatlyreducedwiththeapplicationofaregular
mosphere,upto2Mmabovethephotosphericfloor(Grid6).
chromosphere(Rutten&Uitenbroek 2012). The lack of an
Wefindthatinjectingtheenergyintothechromospherenow
overlyingchromosphericcanopymakesthesmallcorecontri-
butionfromthephotospherevisible. onlycausesstronglinecoreemissionintheHα,CaII8542Å,
Fig. 2 shows contribution functionsfor the Hα and Ca II andMgIIh & kline profiles. Thisisaccompaniedbylarge
8542Ålineswhenanenergyof500ergs/cm3/secisdeposited Dopplershifts due to very strong velocities(>20 km s−1) in
theleadingshockfront.ThestrongDopplervelocitiesappear
between500-700kmabovethephotosphericfloor.Whenthe
duetotheshockfrontinteractingwithtransitionregionwhich
energyis deposited higherin the atmosphere, a strong Ca II
is now at higher column masses. This forces the transition
8542 Å core enhancement is apparent (see Fig. 1). When
regiontoshiftevenlowerintheatmosphere.
the energyis injected lower in the atmosphere,the wing en-
InGrid5,inwhichwevariedtheenergydepositionlocation
hancementbroadensandbecomeslessintenseoverall,asthe
over the photosphere and temperature minimum region, we
energyis being injected into a regionwhere the outer wings
findasimilaratmosphericresponsetothatofFig. 1(Grid2),
areformedoverawiderrangeofheights.
only slightly stronger due to the doubled heating rate. This
canbeseeninFig. 3.
3. MGIIH&KLINEMODELING
Fig. 4 shows the corresponding line profiles synthesised
We have foundthat energydeposited in the 500 - 700 km for the atmospheres shown in Fig. 3. When the energy is
layerresultedinthebestmatchtotypicallyobservedEBline depositedbelowthetemperatureminimumregion(300-500
profiles for the Hα and Ca II 8542 Å lines (e.g. Fig. 5 of kmabovethephotosphericfloor),thereisverylittleresponse
Vissersetal.(2013)). In this Section, we consider the re- inallsynthesisedlines, buta noticeablecontinuumincrease,
sponse of the Mg II h & k lines to similar EB heating. Re- andslightwingenhancementin Hα andCa II 8542Å. Sim-
cent observations with the IRIS instrument hint at enhance- ilar to the quiet Sun model, the best fitting for the Hα and
mentsinthewingsoftheselines(seeFig. 10of(Vissersetal. Ca II 8542 Å line profiles appears when the energy is in-
2015)).WeusetheRHlinesynthesiscode(Uitenbroek 2001; serted around the temperature minimum region (500 - 700
Pereira&Uitenbroek 2015) to calculate the line profiles in km). However, the Mg II h & k lines appear to have only
partial redistribution (PRD). The 2 grids of models run for theirouterwingsshowingenhancement.TheresponseofMg
HαandCaIIintheprevioussectionproducenoenhancement II h & k when the heating is applied between 700 - 900 km
intheMgIIh&klines(Grids1and2). abovethephotosphericfloorismostsimilartothatofstrong
A furthergridof modelswas created, which increases the
4 Reidetal.
∆λ(nm) ∆λ(nm)
−0.6 −0.4 −0.2 0.0 0.2 0.4 0.6 −0.2 −0.1 0.0 0.1 0.2
τν = 1 Ci τν = 1 Ci
v Time = 10.00s v Time = 10.00s
z z
1.5 Iν 1.5 Iν
m) 1.0 m) 1.0
M M
ht ( ht (
g g
Hei Hei
0.5 0.5
0.0 0.0
300 200 100 0 −100 −200 −300 50 0 −50
∆ν (km s−1) ∆ν (km s−1)
Figure2. Left: ContributionfunctionfortheHαline. Right: ContributionfunctionfortheCaII8542Ålineprofile. Darkregionsindicateareasofstrong
contribution. Thegreenlinesshowthelineprofiles. Theredlinesshowtheτ=1location,andthebluedashedlineshowstheverticalvelocityasafunctionof
height.
Figure3. Left: Temperatureprofileacrossthetemperature minimumregionfor1000ergs/cm3/secdeposited atvarious heights, usingthepre-flarestarting
atmosphere.Middle:Verticalvelocityprofiles.Right:Electrondensityprofiles.Thedashedlinesindicaterunswiththeinjectedenergydensityhalved.
observed IRIS bombs (see Fig. 10 in (Vissersetal.2015)). chromospherecauses strong emission, especially in the core
However, the Ca II 8542 Å line profile shows strong core ofCaII8542Å.WhenconsideringtheMgIIh&klinepro-
emission with energy deposited at this height. When halv- files,thequietSunstartingatmosphereisnotviable,asitpro-
ingtheenergydepositionratetotheidealrateidentifiedinthe ducedabackgroundprofileinabsorption.Insertingtheenergy
previoussection,wefindtheenhancementsinthelinesreduce aroundthe temperatureminimum only enhancedthe contin-
slightlyinCaII8542ÅandMgIIh&k,withaslightlylarger uum around these lines. The mid-upper chromosphere was
differentialapparentintheHαlineprofile. thelocationofthemaincontributionoftheMgIIh&klines,
To investigateif a largerdepth rangefor the energydepo- andsoonlybydepositingenergyherecouldonegetavisible
sition is more appropriate, we also ran two larger modelsin responseintheselines,whichcouldovercomethecontinuum
boththequietSunandpre-flareatmospheres(Grids7and8). enhancement. This would then only cause flare-like profiles
These models inject 500 ergs/cm3/sec over ranges of 500 - intheHαandCaII8542Ålinecores.
1000 km and 500 - 1200 km. In all cases, strong core en- A pre-flare, plage-like starting model was used in an at-
hancementswereseeninthesynthesisedCaII8542ÅandHα tempttoovercomethisandpushtheformationtoloweratmo-
lineprofiles. TheMgIIh&klineprofilesappearedtoshow spheric heights. While this was the case, the Hα and Ca II
flare-like profiles with the pre-flare atmosphere, and strong 8542Å line coreswereenhancedin comparisonto the quiet
enhancementinthelinewingsinthequietSunatmosphere. Sunmodel,withtheCaII8542Åbackgroundprofileappear-
ingparticularlyunrealisticincomparisontoobservations.
4. DISCUSSIONANDCONCLUSIONS However,itwas possibleto achieveMg IIh &k line pro-
filessimilartoobservationsbydepositing500ergs/cm3/secat
Wehaveused1-dimensionalradiativehydrodynamicalsim-
700-900 km above the photospheric floor. While the Mg II
ulationsofthesolaratmospheretoinvestigatethelocationand
profiles look similar to IRIS observations, the Ca II 8542 Å
rate of energydeposition required to reproduceEB-like line
cores appear in emission. If the energy is inserted 200 km
profiles. Our findings based on a quiet Sun starting atmo-
lower in the atmosphere (the ideal setup from the quiet Sun
sphere suggest that the location of energydepositionis near
the temperature minimum region, around 600 km above the models), the Hα and Ca II 8542 Å line profiles appear EB-
photospheric floor. We find that placing the energy into the like, with wing emission and no core enhancement, relative
INVESTIGATINGIRIS/ELLERMANBOMBSIN1-DRADIATIVEHYDRODYNAMICS 5
Figure4. Top:MgIIh&klineprofiles,calculatedinPRDfromtheatmospheresinFig. 3. BottomLeft: Hαlineprofiles. BottomRight: CaII8542Åline
profiles.Thedashedlinesindicatethelineprofileswhentheenergydepositionishalved.
tothebackgroundprofile. TheMgIIh&kprofileshowever bytheEuropeanCommissionsFP7CapacitiesProgramunder
appearwithenhancementintheouterwings,muchunlikeob- the GrantAgreement312495. The research leadingto these
servations. results has received funding from the European Communi-
Wehaveshownthatbyconsideringthestartingatmosphere tys Seventh Framework Programme (FP7/2007-2013)under
to bequietSun, we can obtainEB-like syntheticHα andCa grantagreementno. 606862(F-CHROMA).
II 8542 Å line profiles. This results in bi-directional flows
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GridNumber EnergyRate Height(km) Atmosphere Comments
1 100-1000 300-500 QuietSun 300-700ergs/cm3/secbestfitEBprofilesinHα.
2 500 300-1000(200kmstep) QuietSun 500-700kmbestfitEBprofilesinHαandCaII.
3 1000-1x106 300-500 QuietSun All<10,000K.Overwhelmedbycontinuumemissioninalllines.
4 500 1000-2000(200kmstep) QuietSun Flare-likeprofilesinCa&Hα.GoodMgIIresponse.
5 500/1000 300-900(200kmstep) Plage 500-700kmbestfitsEBCa&Hαprofiles.700-900kmbestfitsIBMgIIprofiles.
6 500/1000 1000-2000(200kmstep) Plage Flare-likeprofilesinalllines.
7 500 500-1000 Both StronglinecoreenhancementinCa,Hα.WeakMgIIresponseinQSatmosphere.
8 500 500-1200 Both Cainfullemission,Hαstrongenhancement.GoodMgIIresponseinQSatmosphere.
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