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Transcript of RR Lyrae stars: new discoveries in the OGLE data · RR Lyrae stars: new discoveries in the OGLE...
IAU General Assembly 2015
Focus Meeting 17: Advances in Stellar Physics from Asteroseismology
.
RR Lyrae stars: new discoveries in the OGLE data
Radosław Smolec (CAMK PAN, Warsaw)
Henryka Netzel (Warsaw University)
Igor Soszynski (Warsaw University)
I Warsaw University project
I now OGLE-IV (since 2010)
I more than 100k classical pulsatorsin LMC, SMC and Galactic bulge
photo: www.astrouw.edu.pl
RR Lyrae stars: new discoveries in the OGLE data 1
Optical Gravitational Lensing Experiment, OGLE, 1992–
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
1.2
1.4
5200 5400 5600 5800 6000 6200 6400 6600 6800
∆I [
mag
]
time [d]
Soszynski et al. (2014), Smolec et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 2
Blazhko Effect in double-mode RR Lyr stars
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
1.2
1.4
5200 5400 5600 5800 6000 6200 6400 6600 6800
∆I [
mag
]
time [d]
0.720
0.725
0.730
0.735
0.740
0.745
0.750
0.755
-0.50 -0.40 -0.30 -0.20
P1O
/PF
log PF
OGLE-IV Galactic bulge RRd stars
one, two, three,modulation periods
Soszynski et al. (2014), Smolec et al. (2015)
? majority of the modulatedRRd stars have atypical pe-riod ratio
? multiperiodic modulation ispresent
RR Lyrae stars: new discoveries in the OGLE data 2
Blazhko Effect in double-mode RR Lyr stars
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0 40 80
120
A0
[mm
ag]
F
0 40 80
120
5200 5400 5600 5800 6000 6200 6400 6600 6800 7000
A1
[mm
ag]
time [d]
1O
2
4
6
8
φ 0 [
rad]
F
-4
-2
0
2
5200 5400 5600 5800 6000 6200 6400 6600 6800 7000
φ 1 [
rad]
time [d]
1O
0
10
20
30
A [
mm
ag] PB2=322.9d
0 10 20 30 40
0 0.01 0.02
A [
mm
ag]
frequency [c/d]
PB1=209.8d
0 0.2 0.4 0.6 0.8
A [
rad]
0 0.2 0.4 0.6 0.8
0 0.01 0.02
A [
rad]
frequency [c/d]
0 40 80
120
A0
[mm
ag]
PB2
0 40 80
120
0 1 2
A1
[mm
ag]
phase
PB1
2
4
6
8
φ 0 [
rad]
PB2
-4
-2
0
2
0 1 2
φ 1 [
rad]
phase
PB1
? both radial modes may be modulated with the same period, but
? more commonly, dominant modulation for the fundamental mode has dif-ferent period than dominant modulation for the first overtone
?Smolec et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 3
Blazhko Effect in double-mode RR Lyr stars
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
40
60
80
100
A [
mm
ag]
OGLE-III OGLE-IV
2
3
2500 3500 4500 5500 6500
φ [r
ad]
time [d]
F mode1O mode
? amplitudes and phases of theradial modes vary irregularlyon a long time-scale of a fewhundred or thousand days
? the short-term modulations arealso irregular
Smolec et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 4
Blazhko Effect in double-mode RR Lyr stars
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
40
60
80
100
A [
mm
ag]
OGLE-III OGLE-IV
2
3
2500 3500 4500 5500 6500
φ [r
ad]
time [d]
F mode1O mode
0
40
80
120
A [
mm
ag]
OGLE-III OGLE-IV
F mode1O mode
-2
0
2
4
2500 3500 4500 5500 6500
φ [r
ad]
time [d]
? amplitudes and phases of theradial modes vary irregularlyon a long time-scale of a fewhundred or thousand days
? the short-term modulations arealso irregular
? OGLE-BLG-RRLYR-13442 hasswitched the pulsation mode(RRab→RRd; Soszynski et al.2014)
Smolec et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 4
Blazhko Effect in double-mode RR Lyr stars
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335.Soszynski et al. (2009,-10,-11)
F+2O: 9 stars.Chadid et al. (2009),
.Poretti et al. (2010),
.Benkö et al. (2010),
.Guggenberger et al. (2011)
1O+?: 23 stars.Gruberbauer et al. (2007)
.Olech & Moskalik (2009)
.Soszynski et al. (2009)
.Süveges et al. (2012)
.Moskalik et al. (2011, -15)
.Chadid (2012), Szabo et al. (2014)
.Molnar et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 5
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335.Soszynski et al. (2009,-10,-11)
F+2O: 9 stars.Chadid et al. (2009),
.Poretti et al. (2010),
.Benkö et al. (2010),
.Guggenberger et al. (2011)
1O+?: 170 stars.Gruberbauer et al. (2007)
.Olech & Moskalik (2009)
.Soszynski et al. (2009)
.Süveges et al. (2012)
.Moskalik et al. (2011, -15)
.Chadid (2012), Szabo et al. (2014)
.Molnar et al. (2015)
.Netzel, Smolec & Moskalik (2015a)
RR Lyrae stars: new discoveries in the OGLE data 5
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335.Soszynski et al. (2009,-10,-11)
F+2O: 9 stars.Chadid et al. (2009),
.Poretti et al. (2010),
.Benkö et al. (2010),
.Guggenberger et al. (2011)
1O+?: 171 stars.Gruberbauer et al. (2007)
.Olech & Moskalik (2009)
.Soszynski et al. (2009)
.Süveges et al. (2012)
.Moskalik et al. (2011, -15)
.Chadid (2012), Szabo et al. (2014)
.Molnar et al. (2015)
.Netzel, Smolec & Moskalik (2015a)
.Smolec et al. (2015, Bl-RRd)
RR Lyrae stars: new discoveries in the OGLE data 5
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335.Soszynski et al. (2009,-10,-11)
F+2O: 9 stars.Chadid et al. (2009),
.Poretti et al. (2010),
.Benkö et al. (2010),
.Guggenberger et al. (2011)
1O+?: 189 stars.Gruberbauer et al. (2007)
.Olech & Moskalik (2009)
.Soszynski et al. (2009)
.Süveges et al. (2012)
.Moskalik et al. (2011, -15)
.Chadid (2012), Szabo et al. (2014)
.Molnar et al. (2015)
.Netzel, Smolec & Moskalik (2015a)
.Smolec et al. (2015, Bl-RRd)
.Jurcsik et al. (2015)
RR Lyrae stars: new discoveries in the OGLE data 5
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335.Soszynski et al. (2009,-10,-11)
F+2O: 9 stars.Chadid et al. (2009),
.Poretti et al. (2010),
.Benkö et al. (2010),
.Guggenberger et al. (2011)
1O+?: 304 stars.Gruberbauer et al. (2007)
.Olech & Moskalik (2009)
.Soszynski et al. (2009)
.Süveges et al. (2012)
.Moskalik et al. (2011, -15)
.Chadid (2012), Szabo et al. (2014)
.Molnar et al. (2015)
.Netzel, Smolec & Moskalik (2015a)
.Smolec et al. (2015, Bl-RRd)
.Jurcsik et al. (2015)
.Netzel, Smolec & Moskalik (2015b)
RR Lyrae stars: new discoveries in the OGLE data 5
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.600
0.605
0.610
0.615
0.620
0.625
0.630
0.635
0.640
0.20 0.30 0.40
Px/
P1O
P1O [day]
Galactic bulge, Netzel et al.M3, Jurcsik et al.
• common form of RR Lyr pulsation:93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.600
0.605
0.610
0.615
0.620
0.625
0.630
0.635
0.640
0.20 0.30 0.40
Px/
P1O
P1O [day]
Galactic bulge, Netzel et al.M3, Jurcsik et al.
• common form of RR Lyr pulsation:93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.0
1.0
2.0
3.0
4.0
0.6 0.61 0.62 0.63 0.64P/P1O
OGLE-BLG-RRLYR-06610A (mmag)P1O=0.31623d
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-06802A (mmag)P1O=0.31830d
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-07806A (mmag)P1O=0.31900d
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-08826A (mmag)P1O=0.31251d
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-09126A (mmag)P1O=0.32399d
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-09305A (mmag)P1O=0.30295d • common form of RR Lyr pulsation:
93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.56
0.58
0.6
0.62
0.64
0.66
0.68
0.2 0.25 0.3 0.35 0.4
P4O
/P1O
, P3O
/P1O
P1O [day]
Z=0.0001Z=0.001Z=0.01
• common form of RR Lyr pulsation:93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0
0.002
0.004
0.6 0.61 0.62 0.63 0.64
OGLE-BLG-RRLYR-08597
0
0.002
0.004
1.2 1.22 1.24 1.26 1.28P/P1O
• common form of RR Lyr pulsation:93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.0
1.0
2.0
3.0
4.0
0.6 0.61 0.62 0.63 0.64P/P1O
all data
0.0
1.0
2.0
3.0
4.02013
0.0
1.0
2.0
3.0
4.02012
0.0
1.0
2.0
3.0
4.02011
0.0
1.0
2.0
3.0
4.0OGLE-BLG-RRLYR-07806
2010A (mmag)
P1O=0.31900d • common form of RR Lyr pulsation:93% of RRc/RRd observed from space (13/14)
38% of M3 RRc/RRd stars (Jurcsik et al. 2015)
3% of OGLE-III Galactic bulge stars, but
27% in the two high cadence OGLE-IV fields
• three sequences in the Petersen dia-gram
up to three non-radial modes in a single star
• additional mode(s) must be non-radial
• subharmonics of additional mode(s)are present
• additional modes are non-stationary
Netzel, Smolec & Moskalik (2015a,b)
RR Lyrae stars: new discoveries in the OGLE data 6
Non-radial modes in RR Lyr stars: 0.61–0.63 period ratio
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
F+1O: 1335
F+2O: 9 stars
1O+?: 304 stars
RR Lyrae stars: new discoveries in the OGLE data 7
New class of double-periodic RR Lyr stars: gravity mode pulsation?
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.58
0.60
0.62
0.64
0.66
0.68
0.70
0.72
0.74
0.76
-0.60 -0.50 -0.40 -0.30 -0.20
PS/
PL
log PL
F+1O
F+2O
1O+?
?+1O
F+1O: 1335
F+2O: 9 stars
1O+?: 304 stars
?+1O: 12 stars (11 OGLE+1 Kepler), Netzel, Smolec & Dziembowski (2015)
Period of the additional mode is longer than 1O period. It is longer thanperiod of the (undetected) F mode!
RR Lyrae stars: new discoveries in the OGLE data 7
New class of double-periodic RR Lyr stars: gravity mode pulsation?
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
• dominant pulsation: radial first over-tone
• very narrow range of period ratios
• additional mode is always coherent
• it must be a non-radial mode of gra-vity (or mixed) character
• instability range extends slightly be-low F mode frequency, but no obviousselection mechanism can be propo-sed
Netzel, Smolec & Dziembowski (2015)
RR Lyrae stars: new discoveries in the OGLE data 8
New class of double-periodic RR Lyr stars: gravity mode pulsation?
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015
0.682
0.683
0.684
0.685
0.686
0.687
0.688
0.689
0.690
-0.5 -0.45 -0.4 -0.35 -0.3 -0.25 -0.2
P1O
/Px
log Px
0.68 starsKIC9453114
• dominant pulsation: radial first over-tone
• very narrow range of period ratios
• additional mode is always coherent
• it must be a non-radial mode of gra-vity (or mixed) character
• instability range extends slightly be-low F mode frequency, but no obviousselection mechanism can be propo-sed
Netzel, Smolec & Dziembowski (2015)
RR Lyrae stars: new discoveries in the OGLE data 8
New class of double-periodic RR Lyr stars: gravity mode pulsation?
Honolulu, IAU GA, FM17: Advances in Stellar Physics from Asteroseismology, 12-14.08.2015