The Impact of Suzaku on the Knowledge of Cataclysmic Variablesdaitakei.com/common/files/presentation_cvconf_20110912a.pdf · 1 2 3 1 2 3 4 1 2 3 1 2 3 4. 16/14. 2-2. Dwarf Novae (DNe)

http://photojournal.jpl.nasa.gov/archive/PIA09221.mov

The Impact of Suzaku on the Knowledge of

Cataclysmic Variables

Dai Takei

The Golden Age of CVs and Related Objects, 2011.09.14

Harvard-Smithsonian Center for AstrophysicsRikkyo University

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Acknowledgement

• Suzaku managers and operation members• Hayakawa Satio foundation (travel grant)• My Ph.D. thesis advisers ...

- Shunji Kitamoto- Masahiro Tsujimoto- Jan-Uwe Ness- Jeremy J. Drake

and all concerned ...

(Rikkyo University)(JAXA/ISAS)(ESA/ESAC)

(Harvard CfA)

Vorrei ringraziare gli organizzatori per avermi dato la possibilita` di parlareI would like to thank the organizers for giving me a chance to talk

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Scope & Goal

• Scope : observational results in X-rays- An emphasis on Suzaku results- Results in other wavelengths are not included

• Goal : to convey three ideas- Various fields are covered with Suzaku- Magnetized CVs, Dwarf Novae, Classical Novae, etc.

- Great impacts on the knowledge of CVs- Non-thermal processes with high energy emission

- ASTRO-H has important roles in future- Further improvement of X-ray instruments

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Talk Plan

1.

Suzaku X-ray Mission

2.

Review of Suzaku Results

3.

Suzaku Impact on CVs

4.

Future Outlook

1 2 3 4

1 2 3

1 2 3

Further reading

:• Suzaku Home Page• http://www.astro.isas.jaxa.jp/suzaku/index.html.en

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Talk Plan

1.

Suzaku X-ray Mission

2.

Review of Suzaku Results

3.

Suzaku Impact on CVs

4.

Future Outlook

Further reading

:• Suzaku Home Page• http://www.astro.isas.jaxa.jp/suzaku/index.html.en

～ 3 min

～ 6 min

～ 8 min

～ 6 min

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1-1. What is Suzaku ...?

http://eda.plain.isas.jaxa.jp/suzaku_xoops/modules/newbb/download.php?url=/Bamba_Bamba_Aya.ppt.1149042392000http://www2.gol.com/users/stever/SuzakuKitora.jpg

1

© A. Bamba

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1-1. What is Suzaku ...?

http://eda.plain.isas.jaxa.jp/suzaku_xoops/modules/newbb/download.php?url=/Bamba_Bamba_Aya.ppt.1149042392000http://www2.gol.com/users/stever/SuzakuKitora.jpg

1

© A. Bamba

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1-2. Suzaku X-ray Satellite

• Japan-US joint mission• Launched on July 10, 2005• Low-Earth orbit ...

- altitude ～

570 km- orbital period ～

96 min

http://www.astro.isas.jaxa.jp/suzaku/overview/; http://heasarc.gsfc.nasa.gov/Images/astroe/instruments/astroe2_full_small.jpg; Mitsuda et al. 2007, PASJhttp://eda.plain.isas.jaxa.jp/suzaku_xoops/modules/newbb/download.php?url=/Bamba_Bamba_Aya.ppt.1149042392000

2

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1-2. Suzaku X-ray Satellite

(0,1,2,3)2XIS HXD

(PIN,GSO)XRS

Disable

http://www.astro.isas.jaxa.jp/suzaku/overview/; http://heasarc.gsfc.nasa.gov/Images/astroe/instruments/astroe2_full_small.jpg; Mitsuda et al. 2007, PASJhttp://eda.plain.isas.jaxa.jp/suzaku_xoops/modules/newbb/download.php?url=/Bamba_Bamba_Aya.ppt.1149042392000

61 μsec8 secTiming Res.

4.0 keV (PIN)130 eV @ 6 keVEnergy Res.

N/A2 arcm. (HPD)Spatial Res.

15 ～

600 keV0.2 ～ 12 keVBandpass 62.0 ～

1.0 A

。0.8 ～

0.02 A

。

2

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1-3. Advantages of Suzaku

• Wide-band X-ray observations with ...- high effective areas- medium energy resolutions- low background levels

http://eda.plain.isas.jaxa.jp/suzaku_xoops/modules/newbb/download.php?url=/Bamba_Bamba_Aya.ppt.1149042392000

Diagnoses of emission line spectra

Studies of high energy phenomena

3

‘...> Let

s take a look !

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2. Review of Suzaku Results

1.

Magnetic CVs (Polar, IP)

2.

Dwarf Novae

3.

Classical Novae

Three Ph.D. and 16 papers were producedTwo of them were issued in press releases

1

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2-1. Magnetic CVs

• Ph.D. Thesis- Takayuki Yuasa, 2011

- Suzaku Studies of White Dwarf Stars- and the Galactic X-ray Background Emission

• Refereed Papers- Hayashi et al. 2011, PASJ- Yuasa et al. 2010, A&A- Terada et al. 2010, ApJ- Scaringi et al. 2010, MNRAS- Nobukawa et al. 2009, PASJ- Anzolin et al. 2009, A&A- Terada et al. 2008, PASJ

Yesterday,13:00

Next Talk

Next Talk

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2-1. Magnetic CVs




Yesterday,13:00

Next Talk

Next Talk

WD

Accretion Shock

(fluorescence)

X-ray(thin-thermal)

1.

WD mass2.

Geometry of accretion shocks

3.

Spin period, etc...

Systematic studies wereconducted on magnetic CVs

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2-1. Magnetic CVs




Yesterday,13:00

Next Talk

Next Talk

Main Topic (1)

2

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2-2. Dwarf Novae (DNe)

• Ph.D. Thesis- Shunsaku Okada, 2008

- An Observational Study on the Nature- of the Boundary Layer Plasma in the- Non-Magnetic Cataclysmic Variable SS Cygni

• Refereed Papers- Byckling et al. 2010, MNRAS- Mukai et al. 2009, ApJ- Ishida et al. 2009, PASJ Tomorrow, 9:50

Tomorrow, 9:50

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2-2. Dwarf Novae (DNe)

• Ph.D. Thesis- Shunsaku Okada, 2008

- An Observational Study on the Nature- of the Boundary Layer Plasma in the- Non-Magnetic Cataclysmic Variable SS Cygni

• Refereed Papers- Byckling et al. 2010, MNRAS- Mukai et al. 2009, ApJ- Ishida et al. 2009, PASJ Tomorrow, 9:50

Tomorrow, 9:50

Detailed spectroscopy wasconducted on Dwarf Novae

Accretion Disk

(fluorescence)

X-ray(thin-thermal)

Boundary Layer

WD

3

1.

Phase-induced spectroscopy2.

Partial eclipse

3.

Luminosity classification, etc...

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2-3. Classical Novae (CNe)

• Ph.D. Thesis- Dai Takei, 2011

- An X-ray Study of Classical Novae

• Refereed Papers- Takei et al. 2011, PASJ- Takei and Ness 2010, AN- Takei 2010, Astronomical Herald- Takei et al. 2009, ApJL- Tsujimoto et al. 2009, PASJ- Takei et al. 2008, PASJ

My Thesis

Our Results

4

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My Thesis

Our Results

1.

WD mass2.

Ejecta chemistry

3.

Binary evolution, etc...

Systematic studies wereconducted on Classical Novae

WD

SSS X-ray(photosphere)Hard X-ray(thin-thermal)

Shock ?

4

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My Thesis





Our Results

4

< Suzaku< XMM-Newton

1.

Surveys by amateur astronomers2.

X-ray monitoring with Swift

3.

Deep spectroscopy with Suzaku

Friday,17:00by Dr. Kim Page

X-ray observation of CNe(e.g., V2491 Cyg; Swift)

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My Thesis

Our Results

Main Topic (2)

The golden age of CNe has arrived !!

4

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3. Suzaku Impact on CVs

• Two press releases- Non-thermal pulses from AE Aqr (Magnetic CVs)

- (Terada et al. 2008, PASJ, 60, 387)

- Non-thermal X-rays from V2491 Cyg (CNe)- (Takei et al. 2009, ApJL, 697, 54)

• What is the Suzaku impact ...?

CVs have potential tobe non-thermal sources

1

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3-1. WD Pulsars

• Neutron Star (NS) pulsars vs. WD pulsars- Particle acceleration occurs from NS pulsars- Synchrotron emission from magnetosphere

(e.g., Crab pulsar: Mori et al. 2004, ApJ)

- There should be WD pulsars ...?- Suzaku discovered 33 sec pulses from AE Aqr- Synchrotron emission is a feasible origin

(Terada et al. 2008, PASJ)

2

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3-1. WD Pulsars





2

Neutron star pulsar(X-ray image of Crab pulsar)

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3-1. WD Pulsars





2

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3-1. WD Pulsars





2

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3-1. WD Pulsars





2

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3-1. WD Pulsars





2

X-ray pulses from AE Aqr(Terada et al. 2008, PASJ)

WD

NS

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3-1. WD Pulsars





2

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3-1. WD Pulsars





First discovery of non-thermal X-ray pulsesWDs have potential as particle accelerators

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3-2. Hard X-rays from CNe

• Annihilation signatures from CNe- CNe produce radioactive isotopes

(e.g., Clayton and Hoyle 1974, ApJL)- Hard X-rays are expected in an outburst

(e.g., Gomez-Gomar et al. 1998, MNRAS)- We discovered the signature with Suzaku ...?

(Takei et al. 2009, ApJL)- A model was proposed to explain the result

(Suzuki and Shigeyama 2010, ApJL)

3

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3

e.g., Hernanz et al. 2001Gomez-Gomar et al. 1998

Radioactive Isotope in CNe(proton-rich nuclei)

862 s

158 m

77 d

3.75 y

106

y

Lifetime13N18F7Be

22Na26Al

Isotope

CO,ONe

CO,ONe

CO

ONe

ONe

Novae

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3

e.g., Hernanz et al. 2001Gomez-Gomar et al. 1998

Radioactive Isotope in CNe(proton-rich nuclei)

862 s

158 m

77 d

3.75 y

106

y

Lifetime13N18F7Be

22Na26Al

Isotope

CO,ONe

CO,ONe

CO

ONe

ONe

Novae

EC(10%)

+

(90%)

Na2211

Ne*2210

Ne2210

e+

e-

e

ee-

Annihilation

511 keV

511 keV

Internal Conversion 1.27 MeV

Na : Neutron-deficient nuclei2211

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3

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3

HXD-GSO

XIS

HXD-PIN

Hard X-rays from CNe(Compton Degrad. Model)

22Na > 22Ne

1.27MeV

511KeV

ComptonDegradation

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3

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3

X-ray Spectra of CNe(V2491 Cyg, Day 9)

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3

X-ray Spectra of CNe(V2491 Cyg, Day 9)

(Γ= 0.1 )

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3

(Suzuki & Shigeyama 2010, ApJ)

Suzaku

Compton Degrad. Model(V2491 Cyg, Mejecta

= 10-3

M。).

22Na > 22Ne

1.27MeV

511KeV

ComptonDegradation

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First discovery of high energy phenomenaCNe have potential as non-thermal sources

3

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3

CVs have potential tobe non-thermal sources

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4. Future Outlook

1.

ASTRO-H (Japan-US X-ray mission)

2.

Further studies of CVs

3.

Are CVs origins of cosmic-rays ...?

1

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4-1. ASTRO-H Mission

• Japan-US joint X-ray mission

• Satellite will be launched in 2014

• Advanced X-ray instruments- Telescope

- Detector

http://www.flickr.com/photos/nasaglobalastro/5246115073/sizes/o/in/set-72157625409310900/; http://astro-h.isas.jaxa.jp/doc/080901_NeXT_SAC1.pdf

: HXT

SXT

: SXS

SXI

HXI

SGD

(Bragg-multilayer mirror)

(Lightweight Wolter-I mirror)

(Micro calorimeter)

(Wide-field CCD array)

(Si-CdTe imager)

(Compton camera)

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4-1. ASTRO-H Mission

• Japan-US joint X-ray mission

• Satellite will be launched in 2014

• Advanced X-ray instruments- Telescope

- Detector

http://www.flickr.com/photos/nasaglobalastro/5246115073/sizes/o/in/set-72157625409310900/; http://astro-h.isas.jaxa.jp/doc/080901_NeXT_SAC1.pdf

: HXT

SXT

: SXS

SXI

HXI

SGD

(Bragg-multilayer mirror)

(Lightweight Wolter-I mirror)

(Micro calorimeter)

(Wide-field CCD array)

(Si-CdTe imager)

(Compton camera)

X-ray Instruments onboard ASTRO-H

100 keV 1 MeV0.1 keV 1 keV 10 keV

HXI SGDSXISXS

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4-2. Further Studies of CVs

• Survey of non-thermal emission

- HXI will provide hard X-ray images (>10 keV)> Study of synchrotron emission from CVs

• First discovery of annihilation lines

- SGD has potential to detect 511 keV photons> Study of annihilation processes on CNe

3

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ASTRO-H/HXI(shadow image; 28-33 keV)

Private communication with H. Odaka

Tungsten mask

ASTRO-H/HXI

3.2 cm

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3

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Compton Degrad. Model(V2491 Cyg, Mejecta

= 10-3

M。).

(Suzuki & Shigeyama 2010, ApJ)

ASTRO-H detection limit(100 ksec)

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Research of particle acceleration in our GalaxyApproach to positron factories in the Universe

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4-3. Origins of Cosmic-Rays

• Cosmic-ray electrons & positrons

- Excess was found by PAMERA (Adriani+ 2009)

- New sites of particle accel., or dark matter ?

• Recent progress on CVs

- AE Aqr (Suzaku; Terada+ 2008)

- V2491 Cyg (Suzaku; Takei+ 2009)

- V407 Cyg (Fermi; Abdo+ 2010)

4

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- V407 Cyg (Fermi; Abdo+ 2010)

4

Result of PAMERA(electron & positron excess)

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- V407 Cyg (Fermi; Abdo+ 2010) Friday,18:40 ?by Dr. Takashi Iijima

This Talk

4

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by Dr. Takashi Iijima








- V407 Cyg (Fermi; Abdo+ 2010) Friday,18:40 ?

This Talk

Result of PAMERA(electron & positron excess)

4

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- V407 Cyg (Fermi; Abdo+ 2010) Friday,18:40 ?by Dr. Takashi Iijima

This Talk

CVs are important objects for cosmic-raysThe platinum age of CVs is coming soon !?

4

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Summary

1.

Suzaku made impacts on the CVs science

2.

We found non-thermal X-rays from CNe

3.

ASTRO-H will be bright, like these CVs

Please let me know if you areinterested in this work.

Grazie per la cortese attenzione !!

[email protected]

Documents

The Impact of Suzaku on the Knowledge of Cataclysmic Variablesdaitakei.com/common/files/presentation_cvconf_20110912a.pdf · 1 2 3 1 2 3 4 1 2 3 1 2 3 4. 16/14. 2-2. Dwarf Novae (DNe)