AQUEYE: SCIENTIFIC TARGETS

Bled, 26-28 March 2008

Anna Sponselli

AQUEYE:

SCIENTIFIC TARGETS


Anna 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


Anna 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 )


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• Pulsars are highly magnetized rotating neutron stars

• Accelerated charged particles

emissions in radio, visible, x-ray and -ray domains


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• 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’’


Anna 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


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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 processes2) 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 SPEEDPHOTOMETRY

short time-scale down to which flickering isstill self-similar

vital information about the driving mechanism behind flickering

understanding the physics occurring at much shorter time-scales


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• Object RA(J2000) Dec(J2000) Type <m> Δmorb Pspin (s) Porb (h)• ST LMi 11 05 39.8 +25 06 28.9 P 15.1 (B) 1.8 (B) - 1.898• YY Dra 11 43 38.3 +71 41 20.4 IP 14.0 (V) 2.0 (V) 529.31 3.969• AM CV 12 34 54.6 +37 37 43.4 NL 14.1 (V) 0.1 (V) - 0.286 (17.1 min)• GP Com 13 05 42.9 +18 01 03 NL 15.6 (B) 0.4 (B) - 0.776 (46.6 min)• CT Ser 15 45 39.0 +14 22 32.7 N 16.3 (V) 0.3 (V) - 4.68• DQ Her 18 07 30.3 +45 51 32.6 IP 15.2 (V) 3.5 (V) 71.066 4.647• V533 Her 18 14 20.3 +41 51 21.3 N 14.4 (V) 0.8 (V) 63.63 3.528• AM Her 18 16 13.3 +49 52 04.2 P 12.0 (V) 1.5 (V) - 3.094

• Object RA(J2000) Dec(J2000) Type <m> Δmorb Pspin (s) Porb (h)• WW Cet 00 11 24.8 -11 28 42.7 DN 13.9 (V) 2.2 (V) 591 4.219• V709 Cas 00 28 48.9 +59 17 21.8 IP 14.1 (V) 0.5 (V) 312.75 5.340• RX And 01 04 35.6 +41 17 58.0 DN 14.0 (V) 1.5 (V) - 5.037• XY Ari 02 56 09.0 +19 26 29 IP 13.1 (K) 0.4 (K) 206.298 6.065• GK Per 03 31 11.8 +43 54 16.8 IP 12.8 (V) 0.9 (V) 351.332 47.923• V1159 Ori 05 28 59.5 -03 33 52.8 DN 13.6 (V) 1.8 (V) - 1.492• V405 Aur 05 57 59.3 +53 53 44.9 IP 13.9 (V) 0.7 (V) 545.455 4.143• KR Aur 06 15 43.9 +28 35 08.9 NL 11.3 (B) 2.3 (B) - 3.907• BG CMi 07 31 29.0 +09 56 22.6 IP 14.3 (V) 1.1 (V) 847.03 3.234• PQ Gem 07 51 17.4 +14 44 24.6 IP 14.0 (V) 0.5 (V) 833.42 5.193• EI UMa 08 38 22.0 +48 38 01.7 DN 14.8 (V) 1.2 (V) 741.6 6.434

- P = polar, IP = intermediate polar, N = nova, NL = nova-like, DN = dwarf nova

4-6 APRIL

8-12 OCTOBER


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22-27 OCTOBER

• Object RA(J2000) Dec(J2000) Type <m> Δmorb Pspin (s) Porb (h)

• RX And 01 04 35.6 +41 17 58.0 DN 14.0 (V) 1.5 (V) - 5.037• XY Ari 02 56 09.0 +19 26 29 IP 13.1 (K) 0.4 (K) 206.298 6.065• GK Per 03 31 11.8 +43 54 16.8 IP 12.8 (V) 0.9 (V) 351.332 47.923• V1159 Ori 05 28 59.5 -03 33 52.8 DN 13.6 (V) 1.8 (V) - 1.492• V405 Aur 05 57 59.3 +53 53 44.9 IP 13.9 (V) 0.7 (V) 545.455 4.143• KR Aur 06 15 43.9 +28 35 08.9 NL 11.3 (B) 2.3 (B) - 3.907• BG CMi 07 31 29.0 +09 56 22.6 IP 14.3 (V) 1.1 (V) 847.03 3.234• PQ Gem 07 51 17.4 +14 44 24.6 IP 14.0 (V) 0.5 (V) 833.42 5.193• EI UMa 08 38 22.0 +48 38 01.7 DN 14.8 (V) 1.2 (V) 741.6 6.434• BK Lyn 09 20 11.2 +33 56 42.6 NL 14.5 (V) 2.4 (V) - 1.800• YY Dra 11 43 38.3 +71 41 20.4 IP 14.0 (V) 2.0 (V) 529.31 3.969

P = polar, IP = intermediate polar, N = nova, NL = nova-like, DN = dwarf nova


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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?


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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


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4-6 APRIL

• Object RA Dec Type <m> Δmpuls Period(s) (sec)• HE 1258+0123 13 01 110.5 +01 07 39.7 DAV 16.26 (V) 0.18 (V) 529 - 1092• IU Vir 14 03 57.2 -15 01 10 DAV 15.67 (B) 0.30 (B) 399, 610, 724, 937• TY CrB 16 01 21.2 +36 48 34.3 DAV 14.36 (V) 0.15 (V) 833, complex• V470 Lyr 18 57 30.2 +33 57 25.9 DAV 14.62 (V) 0.06 (V) 259, 292, 557, 739• PT Vul 19 52 28 +25 09 24 DAV 15.12 (V) 0.05 (V) 256

• Object RA Dec Type <m> Δmpuls Period(s) (sec)• ZZ Cet 01 36 13.6 -11 20 32.2 DAV 14.16 (V) 0.01 (V) 213, 274• GD 1400 01 47 21.8 -21 56 51 DAV 15.4 (V) 0.24 (V) 462 - 823 • V411 Tau 04 18 56.5 +27 17 51.4 DAV 15.20 (V) 0.28 (V) 494, 625, 746• V468 Per 04 20 18 +36 16 36 DAV 15.59 (V) 0.22 (V) 910, 1024• V1396 Ori 05 10 13.9 +04 38 44 DAV 15.36 (V) 0.2 (V) 355, 445, 560

DAV = ZZ Cet WD, DBV = V777 Her WD, DOV = GW Vir

8-12 OCTOBER


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22-27 DECEMBER

• Object RA Dec Type <m> Δmpuls Period(s) (sec)• ZZ Cet +01 36 13.6 -11 20 32.2 DAV 14.16 (V) 0.01 (V) 213, 274• V411 Tau 04 18 56.5 +27 17 51.4 DAV 15.20 (V) 0.28 (V) 494, 625, 746• V468 Per 04 20 18 +36 16 36 DAV 15.59 (V) 0.22 (V) 910, 1024• V1396 Ori 05 10 13.9 +04 38 44 DAV 15.36 (V) 0.2 (V) 355, 445, 560• VW Lyn 09 01 48.7 +36 07 07.7 DAV 14.55 (V) 0.07 (V) 350, 481, 592• RY LMi 09 24 16 +35 16 54 DAV 15.50 (V) 0.06 (V) 215, 271, 304• SW LMi 09 57 50 +33 59 42 DBV 17.2 (B) 0.30 (B) 650, complex

DAV = ZZ Cet WD, DBV = V777 Her WD, DOV = GW Vir


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FLARE STARS

• Object RA(J2000) Dec(J2000) <m> TSp• FL Vir 12 33 26.5 +09 01 01 12.50 (V)

dM5.5e/M7• GJ 643 16 55 25.23 -08 19 21.3 11.70 (V) dM3.5• V1054 Oph 16 55 28.76 -08 20 10.8 9.04 (V) dM3e• VB8 (Gl644C) 16 55 35.74 -08 23 36.0 16.70 (V) dM7

• Object RA(J2000) Dec(J2000) <m> TSp• V1005 Ori 04 59 35.1 +01 47 09 10.05 (V) M1Ve• YZ CMi 07 44 43 +03 33.7 11.12 (V) dM4.5°

4-6 APRIL

8-12, 22-27 OTTOBRE

FLARE STARS = variable star which can undergo unpredictable increases in brightness for a few minutes


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PLANETARY NEBULAE PLANETARY NEBULAE astrophysical laser emissions

RA Dec <m>

21 07 01.6 +42 14 10.2 8.8 (V)

NGC 7027 :


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STARS WITH TRANSITING EXOPLANETSobservation 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 with small masses

large mutual distances


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Object RA Dec <m> Porb (day) Mass (MJ)XO-1 16 02 12 +28 10 11 11.3 (V) 3.941534 0.9HD147506 16 20 36 +41 02 53 8.71 (V) 5.63341 8.17HD149026 16 30 29 +38 20 50 8.15 (V) 2.8766 0.36TrES-3 17 52 07 +37 32 46 12.4 (V) 1.30619 1.92TrES-1 19 04 09 +36 37 57 11.79 (V) 3.0300737 0.61TrES-2 19 07 14 +49 18 59 11.41 (V) 2.47063 1.98

Object RA Dec <m> Porb (day) Mass (MJ)WASP-1 00 20 40 +31 59 24 11.79 (V) 2.51997 0.89XO-2 07 48 07 +50 13 33 11.18 (V) 2.615838 0.57

Object RA Dec <m> Porb (day) Mass (MJ)XO-2 07 48 07 +50 13 33 11.18 (V) 2.615838 0.57

4-6 APRIL

8-12 OCTOBER

22-27 DECEMBER

AQUEYE: SCIENTIFIC TARGETS

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