ARAS Spectroscopy - · PDF fileARAS Eruptive Stars Information Letter #13 | 2015-01-31 | 1 /...

ARAS Eruptive Stars Information Letter 13 | 2015-01-31 | 1 25

Novae p 2-3

Nova Cyg 2014 nebular phase - new spectrum by J EdinNova Cen 2013 nebular phaseNova Del 2013 nebular phase

Symbiotics p 4-12

Survey of V694 Mon increasing activity in JanuaryAX Per turns back to quiescent state

An Introduction to CH Cygniby Dr Augustin Skopal p 14-20

MWC 560 = V694 = by Dr Steve Shore p 21-22

Recent publications about eruptive stars p 23-24

ARAS Eruptive StarsInformation letter ndeg 13 2015-01 31-01-2015

ARAS Web pagehttpwwwastrosurfcomaras

ARAS Forumhttpwwwspectro-arascomforum

ARAS listhttpsgroupsyahoocomneogroupsspectro-linfo

ARAS preliminary data basehttpwwwastrosurfcomarasAras_DataBaseDataBasehtm

ARAS BeAMhttparasbeamfreefrlang=en

ARAS Spectroscopy

Contents

Acknowledgements V band light curves from AAVSO photometric data base

Observations of January 2015

Authors F Teyssier S Shore A Skopal P Somogyi D Boyd J Edlin J Guarro


NOVAE

ARAS DATA BASE httpwwwastrosurfcomarasAras_DataBaseNovaehtm

Nova Del 2013 V339 DelMaximum 14-08-2013Days after maximum 535Current mag V 129Delta mag V 85

Nova Cyg 2014 V2659 DelMaximum 09-04-2014Days after maximum 297Current mag V 132Delta mag V 38

Status of current novae

Nova Cen 2013 V1369 CenMaximum 14-12-2013Days after maximum 413Current mag V 993Delta mag V 58


NOVAE

Nova Cyg 2014 = V2659 Cyg

LuminosityMag V = 129 (01-01-2015)Slow decline

SpectroscopyNova Cyg in nebular phase

SpectroscopyNebular spectrum with noticelly [OII] intense

Observers Tim Lester | Christian Buil | Paul Gerlach | Olivier Garde | Franccedilois Teyssier | Jacques Montier | Antonio Garcia | Joan GuarroPaolo Berardi | Franck Boubault | Peter Somogyi | Miguel Rodriguez | F Boubault | O Thizy

ARAS DATA BASE 209 spectra httpwwwastrosurfcomarasAras_DataBaseNovaeNova-Cyg-2014htmWeb Page httpwwwastrosurfcomarasnovaeNovaCyg2014html

PhotometrySlow decline during the nebular phase (04 mag 100 days)Dark squares AAVSOGreen squares Antonio Garcia and Joan Guarro


ARAS DATA BASE | httpwwwastrosurfcomarasAras_DataBaseSymbioticshtm

Symbiotics

Selected list of bright symbiotics stars of interest

Mag V 01-04-2014

Observing

CH Cygni campaignSee Information Letter 11

AX Per returning to quiescent state

Detect high state of V694 Mon -Activity increased in January



CH Cygni campaignSymbiotics

Coordinates (20000)

RA 19 24 330

Dec +50 14 291

B and V light curves in AAVSO databaseNote the decrease of B -V

See details for the campaignpage

CH Cyg at low resolution - J Guarro- Home made spectroscop - R = 800 - 13-12-2014



AX Per OutburstSymbiotics

The prototype Symbiotic AX Per has beendetected in outburst in august 2014 by ANScollaboration See ATel 6382The current mag is about 109 (declining)Spectra of this event are welcome for ARASdata base Data Base AX PerAras topic for exchanges Forum

Coordinates (20000)

RA 01 h 36 m 227 s

Dec +54deg 15rsquo 25rdquo

Mag ~ 1195 31-01-2015




Spectroscopic evolution during the visualdecline throw Joanrsquos SpectraIncrease of [Fe VII] 5726 6087 lines withthe hardening of the radiation (Fig 2)And also increase of [OIII] 4363 decreaseof electronic temperature (Fig 3)

Fig 1 - Comparison of the spectrum between 2014 13th december (Mag V = 113) and 2015 22th january (Mag V = 12)

Fig 2 - [OIII] 4363 Fig 3 - [Fe VII] 6723 and 6087



V694 Mon = MWC 560Symbiotics

Coordinates (20000)

RA 07 h 25 m 512 s

Dec -07deg 44rsquo 08rdquo

Observing detect high stateDaily coverage should be must

See also - Steversquos notes page xxx- Information letter 2014-11 p 16-14

Spectroscopy increasing activityin January

AAVSO - V band light curve

Its a shame we dont have the UV but there are someneat effects there This is one for which it might beinteresting doing low resolution high cadence moni-toring (eg a spectrum every ten minutes for instan-ce) to see if there is some high frequency variabilityanalogous to the flickeringSteve Shorersquos comment (31-01-2015)

2015-01-24847 LISA R = 1100

The maximum velocity of the absorptionin Balmer lines has significantly increased( v max ~ 2600 kms-1)The absorption profile is type A(nr) ac-cording to Iijima (2002) classification




Comparison of spectra between 2014 december 24th (Peter Somogyi Alpy 600) and 2015 January 17th

(Joan Guarro Home made spectroscopShowing the significant evolution of absorptions in Balmer lines (intensity and velocity) Note also thechanges in HeI 5876 Na I D range

Absorptions of Balmer linesScale radial velocity in kmsF Teyssierrsquo spectrum2015-01-24847 LISA R = 1100



ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s

Dec 08deg 53rsquo 52rdquo

ZZ Cmi is a poorly studied star with very few published spectraDavis Boydrsquos spectra (LISA R=1000) show a tiny variation of [O III](2014 Apr And 2015 Jan)



BX Mon | NQ Gem | UV AurSymbiotics


ARAS Data Base for CH CygnihttpwwwastrosurfcomarasAras_DataBaseSymbioticsCHCyghtmSee also former campaign wwwastrosurfcomarassurveyschcygindexhtml

CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291

Current magnitude V = 74 to 76(Flickering)

Field of CH Cygni - Christian Buil - 15-03-2012

Reference stars

Name RA (2000) Dec (20002) Sp Type Mag V EB-V

HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0

MILES Standart for high resolution spectra

Reference for low resolution spectra

Observing

High resolution spectraEshelLHIRES III 2400 lmm ( H alpha)

Low resolution spectra (minimum R = 600)

Send spectraTo francoismathieuteyssier at bboxfr

File name _chcygni_aaaammdd_hhhfitAnd _chcygni_aaaammdd_hhhzip for eShel

Request for observations of the symbiotic star CH Cygni (Dr A Skopal)Symbiotics


ASAS-SN 15bpNew bright transcient discovered by ASAS-SN

Cataclysmics

A Very Bright High-Amplitude CV Candidate Discovered by ASAS-SN

G Simonian A B Danilet K Z Stanek C S Kochanek T W-S Holoien U Basu N Goss J F Beacom(Ohio State) B J Shappee (Hubble Fellow Carnegie Observatories) J L Prieto (Diego Portales MAS) DBersier (LJMU) Subo Dong (KIAA-PKU) P R Wozniak (LANL) J Brimacombe (Coral Towers Observatory)D Szczygiel G Pojmanski (Warsaw University Observatory)on 23 Jan 2015 1750 UT

During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or Assassin) using data fromthe quadruple 14-cm Brutus telescope in Haleakala Hawaii we discovered a new transient source

Object RA (J2000) DEC (J2000) Disc UT Date Disc V magASASSN-15bp 121240410 +04165621 2015-01-2352 119ASASSN-15bp was discovered at V=119 in ``Brutus images taken on 2015-01-2352 but not present(Vgt172) in images taken on 2015-01-2052 At the position of the transient Vizier reports a match to afaint g=205 blue SDSS source as well as a nearby GALEX NUV=209 source Archival observations fromthe Catalina Real-time Transient Survey (CRTS) do not show outbursts but do indicate variability span-ning two magnitudes possibly due to eclipses

Astronomerrsquos telegram 6981

Spectrum of ASASSN 15bp by Peter Somogyi (Alpy 600)Typical spectrum of a CV in outburst


An introduction tothe enigmatic symbiotic star CH Cygniby Dr Augustin Skopal 17

CH Cygni is a particularly intriguing symbiotic star Itis very bright with V between about 6 and 9 magand well placed in the northern hemisphere (delta ~+50 degrees) which makes it a perfect target formultifrequency ground-based observations In addi-tion on the basis of Hipparcos measurements thedistance of CH Cygni was determined to 244 +49-35pc CH Cygni is thus one of the closest symbioticsystems Despite this advantage the nature of itsactivity fundamental parameters and even its basicconfiguration are poorly understood

1 Enigma of the symbiotic activity

The symbiotic phenomenon of CH Cyg has nocounterpart to other symbiotics in any of its mainfeatures Perhaps the best example is its light curve(see Fig 1) whose profile does not resemble thetypical wave-like orbitally-related variations ob-served in the light curves of other classical symbioticstars during quiescent phases Also active phases brightenings flares seen in the light curve are veryheterogeneous and are not comparable in the pro-

file with any other well observed symbiotic starDuring active phases spectrum of CH Cygni developsemission lines of low excited species (eg HI HeI andmetals like FeII TiII CrII [FeII] etc) and a blue con-tinuum with a characteristic temperature of 6ndash10 103

K During quiescent phases the symbiotic phenome-non practically disappears and the spectrum resem-bles that of an M giant Since the discovery by Graff in 1924 CH Cygni wasknown as a rather typical red semiregular variableand used as a standard of the spectral type M6-7IIISymbiotic activity was recorded for the first time atthe beginning of the 1960s by Deutsch (1964 AnnRep Mt Wilson and Palomar obs p 11) who foundin the spectrum of CH Cygni emission lines of HI FeIFeII and [FeII] and a hot blue continuum superposedover the late-type spectrum Why CH Cygni was inac-tive for a long time until ~1960 remains a puzzle inspite of a trial to explain it by the so-called Kozairesonance operating in a special triple-star systems(see below Section 2) The symbiotic-like characterof the spectrum lasted to ~1965 then occurred againduring 1967 ndash 1970 and during 1977 ndash 1986 - the

Fig 1 - U and V light curves of CH Cygni from its first photoelectric measurements to the present (2015) Active phasesstart with an eruption of the hot star an event indicated by an increase of the brightness by 2-3 mag in U so that U ~V The present active phase is characterized with a slow increase of the hot stars brightness on a time-scale of yearsData are from the literature (eg Skopal et al 2012 AN 333 p 242 and references therein) after 20118 they areunpublished


strongest to date recorded active phase Accordingto the light curve profile following episodes of activ-ity were indicated during 1992 ndash 1995 1998 ndash 2000and recently a slow gradual increase in the U lightfrom around 2010 with the latest (December 2014) Umagnitudes of 7-8 signalizes a strong and long-lastingactive phase of CH Cygni (see Fig 1) Each active phase is followed with a pronouncedrapid light variability on the time-scale of minutes tohours appearance of a warm continuum producedby a white dwarfs pseudophotosphere that veilsfeatures of the cool giant continuum mainly from theblue part of the spectrum and a complex structure ofthe emissionabsorption line profiles with signaturesof a high-velocity mass-outflow from the accretor Asa result it was very difficult to determine basic con-figuration of the CH Cygni system and fundamental

parameters (luminosity radii and temperatures) ofits components by standard methods

2 Puzzle of the CH Cygni configurationbinary or triple-star system

Nevertheless after 16 years of intensive observa-tions from the beginning of activity Yamashita ampMaehara (1979 PASJ 31 307) succeeded in search-ing for a reliable periodicity in radial velocities in thered spectrum They suggested the binary model forCH Cygni consisting of a red giant and a white dwarfwith an orbital period of 156 years In the 1980s theelements of the binary model were improved bymore authors (eg Mikolajewski Mikolajewska ampTomov 1987 ApampSS 131 733) and confirmed by the


Figure 2 Radial velocities of absorption components of ionized metals and central absorption of the H-beta line(squares) and neutral metals of the giant component (circles) Corresponding orbital motions of the binary compo-nents are determined by radial velocity curves (lines) The large scatter in measured values is caused by complexand variable line profiles (see below Fig 3) Figure adapted from Skopal et al (1989 BAICz 40 p 333)


radial velocity for the active component Example isshown in Fig 2 A new avenue in the investigation of CH Cygni wasset by Hinkle et al (1993 AJ 105 p 1074) whosuggested a triple-star model on the basis of preciseradial velocity measurements in the infrared spec-trum In their model the inner 21-yr period binary(the symbiotic pair) is orbited by an unseen G-Kdwarf on a 145-yr orbit The triple-star model wasconfirmed and modified by identifying eclipses inthe system which show that all three stars in thesystem are likely to be in coplanar orbits and thatthe star on the long-period orbit is a second giant(Skopal et al 1996 AampA 308 L9) Another modifi-cation of the triple-star model was motivated toexplain the puzzle of the CH Cygni activity why thissystem was inactive for a very long time until 1960(Seppo amp Kiyotaka 1998 AJ 116 p 444) The au-thors proposed that the system consists of an inner21-yr period binary (35 Mcurren red giant + 05 M(Sun)dim star of unknown type) that is orbited by a whitedwarf of mass ~1 Mcurren If the inner orbit is at a highinclination with respect to the white dwarf orbitthen the activity on the white dwarf is driven by theKozai resonance which causes large eccentricity var-iations in the inner binary When the system is in thehigh-eccentricity state the gas is expelled from thered giant causing activity on the white dwarf Intheir model the eccentricity is growing steadilyfrom 1900 (elt01) to 2050 (e~07)which could switch on the activity of CH Cygni fromaround 1960 However later studies of some authors putdoubts to the triple-star model for CH Cygni Hinkleet al (2009 ApJ 692 p 1360) continued in measur-ing of infrared radial velocities and refined orbitalelements of the CH Cygni orbit In this way theyconfirmed the two previously identified periodsand revised their values to 156 +- 01 yr and to205-yr However they suggested that the long pe-riod results from a binary orbit with a 07 solarmasses white dwarf and 2 solar masses giant whilethe shorter period could be caused by non-radialpulsations of the cool giant Thus they concludedthat the CH Cygni system is a 156-yr period binary

and not a triple system In the following studyPedretti et al (2009 MNRAS 397 p 325) analyzedinfrared interferometric observations with the aimto understand the nature of the mysterious 21-yearoscillation in radial velocities Using the InfraredOptical Telescope Array interferometer and theKeck-I telescope they detected asymmetry of theCH Cygni image changes of which correlated withthe 21-yr period found in the radial velocity meas-urements They argued that such the time-depend-ent asymmetry can be modelled either as the orbitof a low-mass companion around the M giant or asan asymmetric 20 change in brightness across theM giant Their analysis suggested that such the fluxoscillation is unlikely to be explained only in term ofnon-radial pulsation As a result they suggestedthat the combined effect of pulsation and the pres-ence of a low-mass companion could explain thebehaviour revealed by the radial velocity curves andthe time-dependent asymmetry of the CH Cyg im-age In addition they did not find any trace of asecond giant companion in their data Thereforethey concluded that if CH Cyg is a typical long periodvariable then these variations could be explainedby the effect of an orbiting low-mass companionaround the M giant ie a triple-star model wherethe M giant with a faint companion is orbited by thewhite dwarf on the 156-yr orbit The subsequentpaper on the basic configuration of the CH Cygnisystem presented the resolved two stellar compo-nents with bispectrum speckle interferometry(Mikolajewska et al 2010 MNRAS 403 L21) In thisway the authors supported the long-period symbi-otic binary composition for CH Cygni Irrespective to these arguments prioritizing thebinary model for the CH Cygni system the minima ndasheclipses ndash measured during the active phase in 1992and 1994 separated just by 21 years located atthe position of the inferior conjunction of the giantin the symbiotic pair (ie the inner binary of theoriginal Hinkles et al (1993) triple-star model) andduring which all signatures of the active star tempo-rary disappeared (the UV continuum as measuredby the IUE satellite and the flickering variability inthe optical) cannot be explained within the long15-yr period symbiotic binary model Therefore in



my opinion the basic stellar configuration of the CHCygni system remains a big mystery

3 On the accretion and ejection by CH Cygni

Basic condition of interaction between the compo-nents of a symbiotic binary is the mass-loss by thecool giant ndash a natural phenomenon of evolved starswith a large radius (ie with a low gravity at theirsurface) and a high luminosity A fraction of the ma-terial lost by the giant is captured by the gravitation-al field of the compact companion and because of aviscosity the material gradually losses its binding en-ergy (kinetic and gravitationally-potential) for the

benefit of a heat which causes its helical trajectoryand increase in temperature towards the accretorThis process forms an accretion disk around the cen-tral star which thus effectively converts the gravita-tionaly-potential energy of the accreting materialinto the (high-energy) radiation CH Cygni belongs toa small group of symbiotics whose total energy out-put during active phases is as small as a few times 1ndash 10 solar luminosities which can be generated solelyby the accretion process onto a white dwarf becauseit is given by the mass and radius of the accretor andthe accretion rate (= amount of mass accreted perunit of time) For the CH Cygni luminosity of ~30 Lcurrenas measured during its 1992-95 activity (see Skopal2005 AampA 440 p 995) a typical accretion rate of10-8 Mcurren per year and the mass of the accretor of ~1Mcurren require the accretors radius of 001 Rcurren whichrepresents a typical value for a white dwarf Thissimple estimate thus confirms the presence of awhite dwarf in CH Cygni as the accretor However the result of accretion process insymbiotic stars and especially in CH Cygni as ob-served during active phases is extremely complex Inmy opinion the most startling features in the linespectrum of CH Cygni developed in 1981 iearoundafter the middle of the strongest activephase (see Fig 1) when variable inverse P-Cygni typeof profiles occurred and were present in the spec-trum to the end of the optical maximum in July 1984Figure 3 shows an example of such the evolution inthe Ti II 4501 A line profile during July-August 1981This is a very rare direct indication of the mass infallto the accretor at simultaneous mass-outflow from itas indicated by the blue-shifted absorption and emis-sion wings seen simultaneously in profiles In spitethat this phenomenon was well documented bymore authors (eg Wallerstein 1983 PASP 95p135 Yoo amp Yamashita 1984 PASJ 36 p 567 Sko-pal et al 1989 BAICz 40 p 333) it has not beendiscussed in more detail and even approached theo-retically Qualitatively we can speculate that theredward-shifted absorption reflects a warping of theinner parts of the disk resulting in re-accretion of alarger fraction of the disk material onto the whitedwarf which then keeps its activity for a long time of


Figure 3 Evolution of the Ti II 4501 A line profile fromJuly 12 (dotted line) to August 7 (solid line) 1981 Verti-cal dot-dashed line represents the position in the spec-trum corrected for the systemic velocity of -58 kms(adapted from Skopal et al 1989 BACz 40 p 333)Red-shifted absorption features thus indicate a massinfall to the central star


years A dramatic change happened after July 1984when the optical brightness dropped by ~15 magthe line profiles displayed very broad emissionwings that could be matched by a spherically sym-metric ionized wind at a high-velocity while in theradio domain highly-collimated bipolar jets wereobserved for the first time (Taylor et al 1986 Na-ture 319 p 38) This situation was probably con-nected with a final bustling re-accretion from thedisk which caused its destruction resulting in disap-pearance of the warm pseudophotosphere (iecaused the drop in the optical brightness) increasedsignificantly accretion rate and thus made the accre-tor to be much hotter as indicated by a shift of theenergy distribution to the ultraviolet and appear-ance of a strong nebular radiation seen in thespectrum for wavelengths gt ~2000 Aring The radiationof such the white dwarf could also more easily driveout the rest of the surrounding material in the formof the ionized wind as indicated by the broad wingsof the lines expanding to 1000 ndash 2500 kms (see Fig4) The total energy of material accreted onto thewhite dwarf at very high rate from the warpinginner disk could not be probably processed by thewhite dwarf only by a standard way as noted aboveBecause of the rotation the infalling material swirl-ing down to the compact accretor throughout itssteep gravitational field has a high angular momen-

tum that has to be conserved In this situation afraction of such the abruptly accreted material canbe accelerated from the vicinity of the accretor toat least its escape velocity and ejected along therotational axes in the form of highly-collimated jetsSimilar jet activity was detected also duringafter1992-98 and 1999-2001 active phases being stilldetectable even during quiescence (2008) at differ-ent spectral domains Especially in the radio by theVLA in the optical by the HST and in the X-rays bythe Chandra satellite Figure 5 shows examples ofthis fascinating phenomenon

4 The present active phase

According to photometric and spectroscopic meas-urements made during 2014 there are no doubtsthat CH Cygni entered a new active phase Usuallythe first indication of an activity is directly given byevolution in the multicolour light curves when thebrightness in U approaches gradually that in V (seeFig 1) Especially in the case of CH Cygni it is impor-tant to measure the object in short wavelengthpassbands because of a dominant contributionfrom the giant in the optical whose radiation is inaddition highly variable Saying this by other wordsit would be difficult to recognize any active phase ofCH Cygni on the basis of only V light curve (eg using

Figure 4 Left During the maximum of activity redward shifted absorption running from ~0 to ~+200 kms was oftenvery pronounced Right After the 19846 drop in the brightness very extended emission wings in hydrogen Balmerlines developed Assuming that they are caused by the kinematics of the ionized hydrogen we can derive the mass-lossrate from the active star to a few times 10-6 Mcurren per year (see Skopal et al 2002 MNRAS 335 1109)



only the visual estimates from AAVSO database)Second photometric indication of activity is repre-sented by rapid light variations on the time-scale ofa few times 1-10 minutes The former reflects agradual increase of radiation produced by the warmwhite dwarf pseudophotosphere that contributespredominately to the shorter wavelength in theoptical while the nature of the latter effect is notunderstood well The problem however is thestarting point of the present activity because thegiants radiation is significant even within the Uband during quiescence and the simultaneous in-crease in V and U can thus reflect only an intrinsicvariation of the giant (see eg the brightening dur-ing 2010-2011 in Fig 1) To answer the questionldquowhen the recent active phase beganrdquo I will modelthe low-resolution spectra (3600 ndash 7500 Aring) to recog-nize when the contribution from the white dwarfpseudophotosphere starts to be recognizable in thespectrum and will determine its parameters (theluminosity and temperature) and their evolutionThis will naturally provoke questions about the fuelrequired to explain the observed energy outputeg at which rate the material has to be accretedand where does it come from Of course that fromthe giant but the giant in the 16-year or 21-yearorbit Spectroscopic observations with a higher res-olution can inform us about the kinematics of theionized and neutral regions where the strongestlines in the spectrum are originated I have in mindmainly evolution in the hydrogen lines of Balmerseries Their presence and evolution in fluxes can bealso helping to answer the primary question aboutthe beginning of the present CH Cygni activity be-cause their emission measure is proportional to theflux of hydrogen ionizing photons that are producedby the white dwarf (no hope to get sufficient flux ofphotons with wavelength lt 912 A ie ionizing hy-drogen atoms from the cool giant) In particular Ihave a hope to obtain an information about theorbital motion of the active star from measuringradial velocities of the central absorption in thehydrogen line profiles (mainly the H-beta and H-

alpha lines) Their origin during quiescent phases ofsymbiotic stars was explained in the last Informa-tion letter (No 12 of 2014) by Steven Shore Howev-er during active phases of symbiotic stars theneutral medium where the absorption and scatter-ing processes attenuate emission in hydrogen linesis located not only around the giant itself but alsoaround the active star in the form of the neutraldisk-like formation As a result an absorption com-ponent can also be created in the `atmosphereabove the white dwarfs (~10000 K warm) pseudo-photosphere which thus follows its orbital motionHowever the real situation is not so ideal Suchabsorption component will be affected by expan-sion of the shell causing a shift and also by intrinsicvariability causing a scatter in radial velocities Inaddition the component from the white dwarfpseudophotosphere has to dominate the central cutoff in the line which depends on the level of activi-ty Altogether to obtain an appropriate result weneed another strong and long-lasting active phasecomparable with that during 1977 ndash 1985 Accord-ing to my experience with light curves of symbioticstars slowly-starting active phases usually keep astronger activity for a longer time Hoping that thiswill be the case also for CH Cygni However now thisknows only CH Cygni and it is really intriguing star

Augustin Skopal29012015




Figure 5 Images of the jet-like structure in CH Cygni Left VLA map at 49 GHz from March 20 1986 (adapted fromCrocker et al 2001 MNRAS 326 p 781) Right Chandra soft (02-2 keV) image with overlaid contours at harderenergies (6-7 keV magenta) and the VLA 5 GHz image (green contours) X-ray observations were carried out on June8-10 2008 and the VLA observations on October 4 2008 (adapted from Karovska et al 2010 ApJ 710 L132)


MWC 560 = V694 Mon = by Dr Steve Shore

12

The designation MWC refers to a catalog of Balmeremission line objects started by Merrill (yes thesame one as the Raman features the diffuse inter-stellar bands and The Lines of the Chemical Elementsin Astronomical Spectra) These were not only origi-nal observations but were also compiled from the HDand other surveys But since the HD was very lowresolution many of the stars were being observedfor the first time in this version Other listings fol-lowed (eg the Luminous Stars in the Milky Way andso on) -- Merrill P W Burwell C G 1943 ApJ 98153 Like SS 433 this was an ``after-thought in asupplementary listing It was also included in the SSlisting

The bizarre behavior of MWC 560 was first noted byBond H E Pier J Pilachowski C Slovak M ampSzkody P 1984 BAAS 16 516 who realized thatthis might be another SS 433-type object althoughcertainly less extreme Then came the full paperTomov T et al 1990 Nature 346 637 showing thatthe absorption features on the Balmer lines displaceby up to -6000 km s-1 The photometric and spectro-scopic monitoring of this object revealed high andlow states times when the lines appeared more likesymbiotic-like spectra than SS 433 and then out-bursts that -- as youve seen from the spectra --happen in very short intervals

The line profile variations are distinctive While de-tached absorption lines are seen in the classical no-vae you hve been observing especially V339 Del andV1369 Cen they are stationary At least the featuresare invariant within the broad absorption line bound-ary In the MWC 560 profiles the features displaceand are on the Balmer lines There are no variationsof the other lines (Fe II for instance) of the sortindicating the cross coupling during the opticallythick stagesOne good set of profiles is shown inhttpwwwkonkolyhucgi-binIBVS6032Another set of profiles from almost a decade earlieris shown inhttpcdsadsu-strasbgfrabs2002A26A391617I

Iijima in this last paper attributes the changes to aprecessing disk While that may be the case there isnothing to indicate that the period is stable (at leastnot now) and this is one reason why monitoring iks souseful Keep in mind that nobody is doing that alament youre heard too often from me

That MWC 560 is somewhere between a symbioticand a microquasar is supported by the detection ofXR emission by Stute M amp Sahai R 2009 AampA 498209 that they attribute to a boundary layer aroundthe WD from which the jet is launched and loqwerenergy (soft) emission that they attribute to the jetitself in its passage through the circumstellar wind ofthe giant The spectrum of the companion is a ``nor-mal M giant there are indications of long termvariations (on timescales of 340 days) that dontseem to be those of a Mira variable so if theyre lessthan periodic this could be an asymptotic giantbranch (massive) companion that is highly evolvedAs far as I know there are no spectra indicating a Liexcess this is one of the signs of deep mixing in suchevolved stars and shell nuclear processing in thedeep envelope of the giant (as we see in V407 Cygwhich might somehow be related)

High cadence photometry shows flickering This isexpected from a disk not a wind since the times-cales are far too short for any dynamical processexpected from the outflow of a giant And a moreimportant indeed essential problem is again withthe jet and its timescales Let me explain that for amoment

In normal wind outflows the velocity gradient israther shallow usually increasing with distance to-ward the terminal velocity in perhaps 10 stellar radiiThe driving depends on the flux from the star so thegradual shift of the lines toward the terminal velocitycauses a saturation of the profiles and the wind stopsaccelerating and coasts In MWC 560 it seems thevelocity gradient is extremely rapid increasing to theterminal velocity is less than one stellar radius(where here that radius is the WD plus its disk not


the giant whose wind is normal) If there is a pulsa-tion the accretion may be irregular even if theres adisk the feeding of that circum-WD environment mayrender it unstable This is not an explosive ejectionof the V40 Cyg or RS Oph sort The accretion seemsto be more or less steady and there is no thermonu-clear runaway In the 1994 paper this was modeledby assuming a stationary outflow that gets ``massloaded once in a while more mass is expelled butwith the same dynamical properties That what a jetwould mean if like SS 433 An alternative is that thereis no loading but that the precession causes the ma-terial to shift from the line of sight In the UV thiswould produce a decrease in the absorption from thejet but perhaps an increase in the opacity of the disk(the disk isnt hot beyond the boundary layer so therecould be a forest of lines like that in an atmosphere)The UV seems to show the same behavior as theoptical lines in that there are resonance lines thatshift with the optical to high velocity (as I said thisisnt seen in other than Balmer lines in the opticalspectrum) That might be due to the optical depth inthe Lyman series

My apologies this is getting extensively detailedThe problem is that unlike the novae and other sym-biotic systems weve been discussing here the obser-vations are few and old in the UV and beyond Thereis no radio emission so the CH Cyg-like jets are notinvolved and the ejection is not like the emissionpeaks seen in Z And In other words we seem tohave here a high mass accreting WD not a black hole(this is a lo mass system) from a high mass loss redgiant with an induced expulsion of matter Thatthere might be instead not jets but something morelike blobs optically thick bubbles is possible but thatwould not explain the UV

This is definitely a system to adopt to follow and toobserve at more than just the Balmer lines

Steve Shore03-02-2015

For a brief bibliography

httpadsabsharvardeduabs1993ApJ409L53M

httpadsabsharvardeduabs2002A26A391617I

httpadsabsharvardeduabs2001A26A377206S

httpadsabsharvardeduabs2007A26A463703Gpulsation with a period of about 340 days

httpadsabsharvardeduabs2011BlgAJ163Zflickering suggest changes in states related to jetactivity their fig 5 suggests a system with multiplestates but the statistics are poor this paperhttpadsabsharvardeduabs1995A26A300769Tinstead this suggests the states are separatehttpadsabsharvardeduabs2005MNRAS3601257MHe 3-1341 an the flickering-jet connection (this is apaper the ARAS observers should read)

and then theres some theoretical modeling of thespectrumhttpadsabsharvardeduabs1994AJ108671S that includes the UV and optical activity states Themain reason I suggest this last one is the set of UVspectra


22


Recent publications

Novae

Symbiotics

The Curious Case of ASAS J174600-23213 an Eclipsing Symbiotic Nova in OutburstStefan Huumlmmerich Sebastiaacuten Otero Patrick Tisserand Klaus BernhardJAAVSO Vol 43 2015httpwwwaavsoorgsitesdefaultfilesjaavsoej295pdf

Wind mass transfer in S-type symbiotic binaries I Focusing by the wind compression modelSkopal A Carikovaacute ZAstronomy amp Astrophysics Volume 573httparxivorgabs14107674

Optical Flickering of the recurrent nova RS Ophiuchi amplitude - flux relationR Zamanov G Latev S Boeva J L Sokoloski K Stoyanov R Bachev B Spassov S Ibryamov G Nikolovhttparxivorgpdf150102628pdf

Photoionization Heating of Nova Ejecta by the Post-Outburst Supersoft SourceTimothy Cunningham William M Wolf Lars Bildstenhttparxivorgpdf150105690pdf

A Light Curve Analysis of Classical Novae Free-free Emission versus Photospheric EmissionHachisu Izumi Kato MarikoThe Astrophysical Journal Volume 798 Issue 2 article id 76 29 pp (2015)httparxivorgabs14107888

An interesting target forsummer nights


Large amplitude flare from symbiotic nova BF Cyg in outburstATel 7013 U Munari (INAF Padova) A Siviero (Univ Padova) S Dallaporta L Buzzi A Vali-

sa G Cherini S Moretti S Tomaselli A Maitan (ANS Collaboration)on 31 Jan 2015 1154 UT

Credential Certification U Munari (ulissemunarioapdinafit)

Subjects Optical Cataclysmic Variable Nova Variables

The symbiotic nova BF Cyg was discovered when it erupted in 1894 peaking at B=97 It remainedclose to maximum for 30 years and starting with 1924 it begun a slow and gradual descent towardquiescence (Leibowitz and Formiggini 2006 MNRAS 366 675) when in August 2006 while atpassing through B=130 it suddenly erupted again (Munari et al 2006 CBET 596) reaching initiallyB=103 and later peaking at B=97 in October 2008 It has remained around maximum ever sincewith the light-curve nicely modulated by the 757 day orbital period

We are intensively monitoring BF Cyg since 2005 both spectroscopically and photometrically Ontop the protracted maximum now lasting for more than 8 years a unexpected large amplitude andfast evolving flare has recently developed It started between 22 Nov 2014 when we measured BFCyg at B=1115 V=1047 Rc=964 Ic=882 and 21 Dec 2014 when BF was already at B=1072V=998 Rc=930 Ic=855 According to our observations the peak brightness occurred around 26January 2015 at B=995 V=944 Rc=903 Ic=845

The spectra largely changed in response to the flare We obtained Echelle spectra of BF Cyg withthe Varese 061m telescope on 7 Aug 2014 (pre-flare) and 28 Jan 2015 (flare peak) and with theAsiago 182m telescope of 6 Jan 2015 (flare rise) Low resolution spectra were obtained with theAsiago 122m on 18 Nov 2014 (pre-flare) 26 Dec 2014 (flare rise) and 31 Jan 2015 (flare peak)Pre-flare spectra were dominated by very strong Balmer continuum and lines in emission andstrong and sharp HeI lines with no P-Cyg associated absorption During the flare rise HeI and NaIlines broadened and developed strong P-Cyg absorptions with terminal velocities around -250kmsec At flare maximum HeI lines and higher Balmer lines turned into pure absorptions withonly Halpha and Hbeta remaining in emission and among the great number of weak FeII and otherlow excitation emission lines only FeII multiplet 42 lines retained a weak P-Cyg absorption compo-nent No high velocity jet feature has appeared in the emission line profiles

Recent publications


Please - respect the procedure- check your spectra BEFORE sending themResolution should be at least R = 500For new transcients supernovae and poorly observed objectsSA spectra at R = 100 are welcomed

1 reduce your data into BeSS file format2 name your file with _novadel2013_yyyymmdd_hhh_Observer novadel2013 name of the nova fixed for this object

Exemple _chcyg_20130802_886_totofit

3 send you spectra to Novae Symbiotics Franccedilois Teyssier Supernovae Christian Builto be included in the ARAS database

Submit your spectraContribution to ARAS data baseFrom 01-01 to 31-01-2015

D BoydJ EdlinJ GuarroP SomogyiF Teyssier

Further information Email francoismathieuteyssier at bboxfr

Download previous issues httpwwwastrosurfcomarasnovaeInformationLetterInformationLetterhtml

V339 Del = Nova Del 2013

About ARAS initiativeAstronomical Ring for Access to Spectroscopy (ARAS) is an informal group of volunteers whoaim to promote cooperation between professional and amateur astronomers in the field ofspectroscopy

To this end ARAS has prepared the following roadmap

bull Identify centers of interest for spectroscopic observation which could lead to useful effec-tive and motivating cooperation between professional and amateur astronomersbull Help develop the tools required to transform this cooperation into action (ie by publishingspectrograph building plans organizing group purchasing to reduce costs developing andvalidating observation protocols managing a data base identifying available resources inprofessional observatories (hardware observation time) etcbullDevelop an awareness and education policy for amateur astronomers through trainingsessions the organization of proam seminars by publishing documents (web pages) manag-ing a forum etcbull Encourage observers to use the spectrographs available in mission observatories and pro-mote collaboration between experts particularly variable star expertsbull Create a global observation network

By decoding what light says to us spectroscopy is the most productive field in astronomy It isnow entering the amateur world enabling amateurs to open the doors of astrophysics Whynot join us and be one of the pioneers

Be NewsletterPrevious issues httpwwwastrosurfcomarassurveysbeactuindexhtm

Searching for new Be StarsAndrew Smith and Thierry LemoultNew ARAS Pagehttpwwwastrosurfcomarasbe_candidateauto-be-candidatehtml

T Tauri observations upon the request of Henz Moritz Guenther(Harvard-Smithsonian Center for Astrophysics)httpwwwspectro-arascomforumviewtopicphpf=5ampt=1033Almost 200 spectra acquiredhttpwwwastrosurfcomarasAras_DataBaseTtauriT_TauTTauhtm

Comet C2014_Q2 LOVEJOY30 spectra gathered in ARAS data basehttpwwwastrosurfcomarasAras_DataBaseCometsCometsCometshtm


NOVAE

ARAS DATA BASE httpwwwastrosurfcomarasAras_DataBaseNovaehtm

Nova Del 2013 V339 DelMaximum 14-08-2013Days after maximum 535Current mag V 129Delta mag V 85

Nova Cyg 2014 V2659 DelMaximum 09-04-2014Days after maximum 297Current mag V 132Delta mag V 38

Status of current novae

Nova Cen 2013 V1369 CenMaximum 14-12-2013Days after maximum 413Current mag V 993Delta mag V 58


NOVAE










Symbiotics


Mag V 01-04-2014

Observing







Coordinates (20000)

RA 19 24 330

Dec +50 14 291








Coordinates (20000)

RA 01 h 36 m 227 s


Mag ~ 1195 31-01-2015










Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications




















NOVAE










Symbiotics


Mag V 01-04-2014

Observing







Coordinates (20000)

RA 19 24 330

Dec +50 14 291








Coordinates (20000)

RA 01 h 36 m 227 s


Mag ~ 1195 31-01-2015










Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications





















Symbiotics


Mag V 01-04-2014

Observing







Coordinates (20000)

RA 19 24 330

Dec +50 14 291








Coordinates (20000)

RA 01 h 36 m 227 s


Mag ~ 1195 31-01-2015










Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications






















Coordinates (20000)

RA 19 24 330

Dec +50 14 291








Coordinates (20000)

RA 01 h 36 m 227 s


Mag ~ 1195 31-01-2015










Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications























Coordinates (20000)

RA 01 h 36 m 227 s


Mag ~ 1195 31-01-2015










Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications




























Coordinates (20000)

RA 07 h 25 m 512 s







2015-01-24847 LISA R = 1100










ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications



























ZZ CMiSymbiotics

Coordinates (20000)

RA 07 h 24 m 139 s








CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications
























CH Cygni

Coordinates (20000)

RA 19 24 33

Dec +54 14 291



Reference stars


HD 192640 2014319 +3648227 A2V 496 0026


HD 183534 192742 +521914 A1V 57 0



Observing








Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications





















Cataclysmics


















































12





















22


Recent publications

Novae

Symbiotics















Recent publications






























































12





















22


Recent publications

Novae

Symbiotics















Recent publications
































22


Recent publications

Novae

Symbiotics















Recent publications




















Recent publications

Novae

Symbiotics















Recent publications



























Recent publications



















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