Bled, 26-28 March 2008Anna Sponselli AQUEYE: SCIENTIFIC TARGETS.

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Presentation transcript:

Bled, March 2008Anna Sponselli AQUEYE: SCIENTIFIC TARGETS

Bled, March 2008Anna Sponselli Aqueye: ultrafast photometer Exploitation of high time resolution to study high speed astrophysical phenomena in: Pulsars Cataclysmic variables X-ray binaries Pulsating white dwarfs Pulsating neutron stars Flare stars Planetary nebulae Stars with transiting exoplanets

Bled, March 2008Anna Sponselli PULSAR Formation by a supernova explosion Neutron star extremely high density extremely high rotational velocity (periods range from 1.5 ms to 8.5 s ) intense magnetic field (typically in the range of 10^8 - 10^12 gauss )

Bled, March 2008Anna Sponselli Pulsars are highly magnetized rotating neutron stars Accelerated charged particles emissions in radio, visible, x-ray and  - ray domains

Bled, March 2008Anna Sponselli Lighthouse effect extraordinarily rapid and stable rotation pulsed nature very regular rotation period (the regularity of pulsation is as precise as an atomic clock) pulsars as useful instrument for Aqueye’s calibration

Crab Pulsar The first pulsar discovered (1968) Remnant of AD1054 supernova It lies in the Crab Nebula (M1) Period: P= 33 ms Delay: 36ns /day The brightest optical pulsar we know Double pulse per rotation in visible, X-ray and  -ray domains The most energetic pulsar we know Right ascension: 05h 34m 31.97s Declination: +22° 00’ 52.1’’

Bled, March 2008Anna Sponselli CATACLYSMIC VARIABLES CVs = binary systems in which a late-type secondary star fills the Roche lobe and transfers matter onto a white dwarf (WF) CLASSIFICATION ACCORDING TO THE MAGNETIC BEHAVIOUR: 1) non-magnetic systems

Bled, March 2008Anna Sponselli 2) Intermediate- Polars ( DQ Herculis stars) 3) Polars (AM herculis stars)

CVs’ flickering FLICKERING = stochastic brightness variations Time scale : dozen minutes less than a second Amplitudes : a few tenths of magnitude magnitude scale Fig: lightcurve of V709 Cas (Tamburini et al., in preparation) flickering as a continuous series of overlapping flares and bursts in the light curves of CVs with random variability

WHY IS FLICKERING IMPORTANT? 1) it’s a fundamental signature of accretion processes 2) it represents a significant fraction of the total luminosity of the source OPEN QUESTIONS : 1) what’s the exact physical nature? 2) is flickering a self-similar process also at very small scales? HIGH SPEED PHOTOMETRY short time-scale down to which flickering is still self-similar vital information about the driving mechanism behind flickering understanding the physics occurring at much shorter time-scales

Bled, March 2008Anna Sponselli ObjectRA(J2000)Dec(J2000)Type ΔmorbPspin (s) Porb (h) ST LMi P15.1 (B) 1.8 (B) YY Dra IP14.0 (V) 2.0 (V) AM CV NL14.1 (V) 0.1 (V) (17.1 min) GP Com NL15.6 (B) 0.4 (B) (46.6 min) CT Ser N16.3 (V) 0.3 (V) DQ Her IP15.2 (V) 3.5 (V) V533 Her N14.4 (V) 0.8 (V) AM Her P12.0 (V) 1.5 (V) ObjectRA(J2000)Dec(J2000)Type ΔmorbPspin (s)Porb (h) WW Cet DN13.9 (V) 2.2 (V) V709 Cas IP14.1 (V) 0.5 (V) RX And DN14.0 (V) 1.5 (V) XY Ari IP13.1 (K) 0.4 (K) GK Per IP12.8 (V)0.9 (V) V1159 Ori DN13.6 (V)1.8 (V) V405 Aur IP13.9 (V) 0.7 (V) KR Aur NL11.3 (B)2.3 (B) BG CMi IP14.3 (V) 1.1 (V) PQ Gem IP14.0 (V)0.5 (V) EI UMa DN14.8 (V)1.2 (V) P = polar, IP = intermediate polar, N = nova, NL = nova-like, DN = dwarf nova 4-6 APRIL 8-12 OCTOBER

Bled, March 2008Anna Sponselli OCTOBER ObjectRA(J2000)Dec(J2000)Type ΔmorbPspin (s)Porb (h) RX And DN14.0 (V) 1.5 (V) XY Ari IP13.1 (K) 0.4 (K) GK Per IP12.8 (V)0.9 (V) V1159 Ori DN13.6 (V)1.8 (V) V405 Aur IP13.9 (V) 0.7 (V) KR Aur NL11.3 (B)2.3 (B) BG CMi IP14.3 (V) 1.1 (V) PQ Gem IP14.0 (V)0.5 (V) EI UMa DN14.8 (V)1.2 (V) BK Lyn NL14.5 (V)2.4 (V) YY Dra IP14.0 (V)2.0 (V) P = polar, IP = intermediate polar, N = nova, NL = nova-like, DN = dwarf nova

Bled, March 2008Anna Sponselli QPOs (Quasi Periodic Oscillations) QPOs = quasi coherent variabilities about certain frequencies Main sources: Low Mass X-Ray Binaries Probable emission ‘s cause: shocked wave created on the accretion disk Why are we interested in? to understand the innermost regions of accretion disks of the central compact objects What sort of variation with time could cause a QPO?

Bled, March 2008Anna Sponselli PULSATING WHITE DWARFS and NEUTRON STARS Luminosity varitions due to radial and non-radial pulsations: Oscillations time-scale: white dwarfs  100–1000 ms neutron stars  100  s superposition of vibrational modes light output variations asteroseismological evidence about the interiors of the star

Bled, March 2008Anna Sponselli 4-6 APRIL ObjectRADecType ΔmpulsPeriod(s) (sec) HE DAV16.26 (V)0.18 (V) IU Vir DAV15.67 (B)0.30 (B)399, 610, 724, 937 TY CrB DAV14.36 (V)0.15 (V) 833, complex V470 Lyr DAV14.62 (V)0.06 (V)259, 292, 557, 739 PT Vul DAV15.12 (V)0.05 (V)256 ObjectRADecType ΔmpulsPeriod(s) (sec) ZZ Cet DAV14.16 (V)0.01 (V)213, 274 GD DAV15.4 (V)0.24 (V) V411 Tau DAV15.20 (V)0.28 (V)494, 625, 746 V468 Per DAV15.59 (V)0.22 (V)910, 1024 V1396 Ori DAV15.36 (V)0.2 (V)355, 445, 560 DAV = ZZ Cet WD, DBV = V777 Her WD, DOV = GW Vir 8-12 OCTOBER

Bled, March 2008Anna Sponselli DECEMBER Object RADecType ΔmpulsPeriod(s) (sec) ZZ Cet DAV14.16 (V)0.01 (V)213, 274 V411 Tau DAV15.20 (V)0.28 (V)494, 625, 746 V468 Per DAV15.59 (V)0.22 (V)910, 1024 V1396 Ori DAV15.36 (V)0.2 (V)355, 445, 560 VW Lyn DAV14.55 (V)0.07 (V)350, 481, 592 RY LMi DAV15.50 (V)0.06 (V)215, 271, 304 SW LMi DBV17.2 (B)0.30 (B) 650, complex DAV = ZZ Cet WD, DBV = V777 Her WD, DOV = GW Vir

Bled, March 2008Anna Sponselli FLARE STARS ObjectRA(J2000)Dec(J2000) TSp FL Vir (V)dM5.5e/M7 GJ (V)dM3.5 V1054 Oph (V)dM3e VB8 (Gl644C) (V)dM7 ObjectRA(J2000)Dec(J2000) TSp V1005 Ori (V)M1Ve YZ CMi (V)dM4.5° 4-6 APRIL 8-12, OTTOBRE FLARE STARS = variable star which can undergo unpredictable increases in brightness for a few minutes

Bled, March 2008Anna Sponselli PLANETARY NEBULAE PLANETARY NEBULAE astrophysical laser emissions RA Dec (V) NGC 7027 :

Bled, March 2008Anna Sponselli STARS WITH TRANSITING EXOPLANETS observation of planetary transit (for a large time span!) accurate evaluation of the transit starting time observation of TTVs (Transit Timing Variations) detection of other exoplanets orbiting around the same parent star high time resolution detection of companion planets withsmall masses large mutual distances

Bled, March 2008Anna Sponselli ObjectRA Dec Porb (day)Mass (MJ) XO (V) HD (V) HD (V) TrES (V) TrES (V) TrES (V) ObjectRADec Porb (day)Mass (MJ) WASP (V) XO (V) ObjectRADec Porb (day)Mass (MJ) XO (V) APRIL 8-12 OCTOBER DECEMBER