You will be presented with the full text of a science research paper. Please write an abstract for this paper. Your response should include the abstract and no additional text.

Paper text:
classical novae belong to wide class of cataclysmic variables characterized by such commonly features as accretion from the roche lobe filling star to its compact companion ( most often white dwarf ) and by outbursts connected with rapid rise in brightness .
location of accretion material depends on angular momentum distribution and on magnetic field of primary . in most cases ,
stream of matter forms keplerian disc around white dwarf before fall onto its surface . in some systems with the magnetic white dwarf
, called intermediate polar , field is strong enough ( @xmath1 ) to allow material at the outer edge of disc to become magnetically controlled .
accretion can be channeled by bipolar magnetic field on small fraction of primary surface near poles .
both hot regions are sources of anisotropy of emission observed during rotation of white dwarf in x - ray and optical .    here
we present observations of the fast nova v2467 cygni , which was discovered by ahikigo tago in march 2007 at 7.4 mag @xcite .
about twenty days after outburst , extremely strong oi line at 8446@xmath2 was presented in spectra as result of overabundance of oxygen @xcite . during the transition phase , which was started in april , six quasiperiodic oscillations with period from 19 to 25 days and amplitude
about 0.7 mag were observed @xcite .
one year after this , @xcite reported that v2467 cygni is a soft x - ray source and blackbody fitted to its spectra gave parameter kt=34ev .
we obtained our photometric data using the cassegrain 60 cm telescope with sbig stl-1001 camera located in piwnice observatory near torun .
the data was collected during two observational seasons from 12 april 2007 to 28 may 2007 and from 25 june to 23 october 2008 and include mesurements taken with @xmath0 filters to construct long - term light curve . at the same time
, we carried out thirty one - night monitorings to find short time scale variability mainly in v and @xmath3 passband in 2007 and of white light in 2008 .
first search results was presented in @xcite and are agreeable with the one presented below .
transition phase of this nova started about one month after outburst when nova faded about 4 magnitudes . in this time , we monitored this star about 30 hours in @xmath3 and 24 hours in v passband .
we analysed data in two filters separately with fourier methods .
the best fitted periods were 3.46.5 min and 3.40.5 min in @xmath3 and v respectively .      in 2008 , over year after outburst nova was too faint to observe with our telescope and with filters , so we observed white light . in all
, we collected 22 hours of observations which showed two significal variabilities .
we confirm that longer variability , about 3.45.5 min , was observed also in 2007 .
our attention was concentrated on stable changes with period about 40 minutes and amplitude about 0.15 mag .
we do nt have any evindence for exsist changes with this period in 2007 data .
this period is too short to connect its with orbital motion .
we used timing methods on maximas to check if this changes are coherent . on base of this measurements we constructed o - c diagram and computed ephemeris @xmath4 .
we completed x - ray data obtained in september 2008 using swift satellite include 1500 second of observation .
eight points , each include information about several minutes of expositions , were phased with ephemeris showed above .
we attached to single points also errorbar connected with exposition time ( x - axis ) and range from maximum and minimum counts rate ( y - axis ) .
we found short coherent period in optical light curve and confirm that there changes are also visible in x - ray .
our colour light curve show that amplitude of short variations increase in longer wavelength , so can not be connected with disc instabillity or with pulsations of white dwarf .
we can explain it with intermediate polar model when magnetic field have influence on accretion near white dwarf .
this work was supported by the polish mnisw grant n203 018 32/2338 .              _
e. swierczynski _ :
nova had faded quickly about 4 magnitudes to the point when we could observed radiation from the star itself . in the same time
, v2467 cygni was entering brightness oscilations during transition phase with period from 19 to 25 days .      _
e. swierczynski _ : in fact , we observed short variability as superposition of orbital motion and rotaion of white dwarf . in periodogram we can see sign of beat period but not clearly .
we have not any spectra obtainted in this time .
we present the results of unfiltered and @xmath0 band ccd photometry fast nova v2467cyg . 
 our analysis of the data gives two distinct frequencies corresponding to periods of  3.8h and  35 min . 
 the observed light curve of v2467 cyg is typical for an intermediate polar .