One of my favorite“Manga”
placesat Kyoto
MuseumManga-like portrait (1000yen, weekend)

Fushimi Inari

Diversity and Evolutionof Neutron Stars
and Magnetars

Torii leadnig to the inner shrine

Teruaki Enoto
NASA/GSFC
and
RIKEN

X-ray Satellite
SuzakuFox

1

Diversity of Neutron Star; Energy Source
Rotational Energy
Majority of observed NSs

Radio Pulsar
Millisecond Pulsar

Thermal Energy
NS cooling

Compact Central Object
X-ray Dim Isolated NS

Accretion Energy
EoS Measurement

High Mass X-ray Binary
Low Mass X-ray binary

Magnetic Energy

B~1014-15 G

Today’s talkSoft Gamma Repeater
Anomalous X-ray Pulsar
2

Diversity of Neutron Stars
Magnetars

Birth!!

1014

1013

Soft Gamma Repeater (SGR)
Anomalous X-ray Pulsar (AXP)

Binary X-ray Pulsar

Crab-like pulsar

1012 G

1012
1011

em

iss

io

n

Radio pulsar

Distributed due totorque from accretion

di

o

1010

ms pulsar

109

d

of

ra

Rotation-powered
Accretion-powered
Magnetically-powered
Magnetically-powered

En

Surface Magnetic Field (Gauss)

P~2-11 sec, Pdot~10-12-10 s/s

X-ray burster
0.001

0.01

0.1

1

10

Observationally, magnetars are quite
different from nominal radio pulsars.

100

1000

Rotation Period (sec)3

Properties of Magnetars
Soft Gamma Repeater

Anomalous X-ray Pulsar

Giant Flare SGR 1806-20 (2004)

Bright X-ray source (w SNR)

-1 -1
X-ray
count
(0.5
sec)
X⥺࢝࢘ࣥࢺ(0.5 ⛊)fireball?
10

4

L > 8.3x1044 erg/s

Pulse thermal emission
from NS surface

0.35 sec(c) Duncan

103
102
10

1E 1841-045 (SNR Kes 73)

E = 1.2x1044 erg(kT~20 keV)

Hurley+07
100

Chandra Image (c)CXO

200

300

Time ⛊
(sec)
᫬้

400
Morii+10• Dipole magnetic field Bd~1014-15 G via P-Pdot measurements• Supper Eddington giant flares, short bursts, and X-ray outbursts• Distinctive soft and hard X-ray spectra• Connection to extra-galactic events (GRBs etc)4Persistent X-ray Luminosity of SGR/AXP・LX / Esd (Spin-down Luminosity)104
1E1841

J1708

Energy Source?

4U0142

1E2259

SGR0526
J0100
SGR1900
1E1547
SGR1806
SGR0501
1E1048

100

J1647
・

Lx = Esd

1
J1714

J1622

Crab Pulsar

0.01

XTEJ1810

Enough Rotation Energy

SGR1627
PSR 1509-58

Geminga

Enoto+12

10í

0.1

1

10

103

104

Characteristic Age (τc)
Lx >> Spin-down Esd, no evidence for a binary companion (e.g., Kaspi+99)
Magnetars hypothesis; Magnetically-powered Pulsars? (Thompson & Duncan, 95)5

Magnetar Multi-wavelength Emissions
AXP 4U 0142+61 (Persistently Bright)

Enoto+11

Soft and hard X-rays areobservational window !!
Suzaku can cover 0.2-600 keV

No radio emission

Pulsed thermal emission

Pulsed hard X-rays

Photon splitting in high-B
suppresses the e+/e- paircreation and radio emission?

from hot NS surface.
Quasi-BB kT ~ 0.3 keVheated by the interior field

Discovered by INTEGRAL
hard photon index Γ~1
upper limit >750 keV
6Discoveries of Transient Magnetars
160°

140°

120°

100°

80°

60°

40°

20°

0°

SGR 1833-0832

2010

G.C.

Swift J1834-0846
Perseus

SGR 0501+4516

2008

2011

SGR 0418+5719

2009

Sagit. Scutum

-20°


Olausen& Kaspi, 2013
SGR
1806-20
1 RXS J1708-40



180°

1E 1841-045

-40°

-80°

-60°

-100°



Swift J1822-1606


1E
1547.0-5408



Crux Carina


2011



-140° -160° 20°
w


10° gr
m


p

0° ra

w

-10° tr

2008, 2009



Norma

-120°

2006









-20°

SGR 1627-41


CXOI J1647-45


2008




th

Swift launch

SGR 1900+14

4U 0142+61

The McGill Magne









1. New magnetars have been discovered, 1-2 new per year
Figure 1. Number of confirmed magnetars discovered over time.
Labelsin italics bursts
indicate the source
was either
discovered or later
Swift satellite (for the GRB) detects
short
from
magnetars.
detected by an all-sky X-ray/soft gamma-ray burst monitor. The
dashed and dot-dashed lines mark the launches of Swift in 2005
X-ray, optical, and radio follow-up andobservations
within a week.
Fermi in 2008, respectively.
Bright new X-ray source are confirmed with multiple short bursts.
which were later detected (and therefore could have been
discovered)by one, arethought.
highlighted in italics, for this rea2. Magnetar population is much larger than we
previously
son.


Many known magnetars have thus been found via theirbursting behavior, which raises an important point regarding how they are named. Because burst monitors
have tended to find them, magnetars have often been
named with the designation “SGR” in recent years (seeTables). We argue strongly that this naming convention requires amendment because as discussed in thiswork and extensively elsewhere (e.g. Gavriil et al. 2002;
Kaspi et al. 2003; Woods & Thompson 2006; Mereghetti

Challenge to provide a more unified characterization !!

K
w
ta
ta
J
ti
an
b
T
ta
p
th
b

A
lo
in
re
ti
w
sk
eff
of
sc
lu
co
b
K
7

Co

1

0.5

0
X-ray
Outburst
of
AXP
1E
1547.0-5408(1)-0.6 -0.4 -0.2
0
0.2
0.4
0.6
-0.6 -0.4 -0.2
0
0.2

0.4

40
4
10
30

2009Burst-8
January 22 Suzaku/WAM

Burst-7

3 hour

20
103
10

04:00

08:00

4 hours

XI0 2.0-10.0 keV

12:00
0
100
10

Enoto+12

PIN 10.0-70.0 keV

40

Light Curve

16:00

0

20:00

(a4)10.0-70.0
PIN
keV(1) CutPL

Enoto+12(2) 2BB

5
10

Crab Nebula

ï

20

0
31

GSO 50-150 keV

2

20

Suzaku/HXD-WAM

5

00:00
0

60

10

XI0 2.0-10.0 keV

ï

105

-2 s-1 cm-1 )keV
keV2keVcm(Photons
keV

Count Rate (cnt/s)
Rate (cnt/16 ms)
s-1)-1
Count (15.6 ms)-1 Count (15.6 ms)-1 カウントレート
Count (15.6 ms)(cntsTime (s)Known as a fast rotation faint
AXP (P~2 sec)

0.6
Time (s)200 ms
10

-0.6

-0.4

-0.2

0

0.2

0.4

0.6 (sec)
Time (s)Spectrum

2
10.1

0

GSO 50-150 keV

01-0.6 1 -0.4

10
-0.2

10
0 (keV)0.2
Energy100
100

Energy (keV)0.4

0.6
Time (s)Feature1: Recurrent Bright Short Burst
Figure5. Light
curves ms,of theindividual short
events spectrum
detected by
the
Suzak
Duration~100-500(Empirically)
Twoburst
blackbody(kT~ present
4, 11 keV)refer to those obtained with XIS0, with HXD-PIN, and with HXD-GSO, in the 2–10, 10–70
8
is 15.6 msec.

X-ray Outburst of AXP 1E 1547.0-5408 (2)-1-2-2))cm
レート (cnts s-1) Absorbed
X ⥺ࣇࣛࢵࢡࢫ
Flux (erg (ergs-1 scm

Count
Rate (cnt/s)
カウントレート(cnts s-1)

Known as a fast rotation faint AXP (P~2 sec)
2009 January 22 Suzaku/WAM

105

3 hour104

Suzaku/HXD-WAM

4 hours

103
00:00

04:00

08:00

12:00

16:00

20:00

10-8
10-9
10-10
10-11

Swift/XRT

Thermal X-rays (2-10 keV)

6 monthSuzaku/XIS

Suzaku ToO

Suzaku follow-up

10-12
10

-13

1 year

1 mCrab level

Sep
2007

Mar
2008

Sep
2008

Mar
2009

Sep
2009

Mar
2010

Sep
2010

Mar
2011

TE+11
Sep
2011

105

Suzaku/HXD-WAM
Feature2: Persistent X-ray becomes3 hourbrighter by 2-3 ordersof magnitude.
1049

X-ray Outburst of AXP 1E 1547.0-5408 (3)Suzaku ToO Observation 2009 January (33 ks)

keV2 (Photons cmï sï keVï)1

Hard Comp.

Thermal (surface)0.1

Γ ~ 1.5

kT ~ 0.7 keV
.1)
0
+
,
1
1 (-0.

0.01

1
Γ ~ 1.

10ï

Iwahashi & TE et al.+2013
consistent with Kuiper+201210ï

kT ~ 0.65 keV(2.9 km)10ï

kT~0.4 keV

10ï12006 XMM Observation(Gelfand+07)
10100
Energy (keV)

Enoto+09

Hard X-rays were clearly discovered during the magnetar outburst with Suzaku.

Feature2: Persistent X-ray becomes brighter by 2-3 orders of magnitude
Both components (soft thermal + hard X-rays) become brighter
10

X-ray Outburst of AXP 1E 1547.0-5408 (4)Before Burst

2009
Outburst

X-ray countrate

4-34 keV

Kuiper+12

11-34 keV
After Burst△(Spin Frequency)
4-34 keV

11-34 keV

Feature3: Pulse profile changes at the outburst( ˙ / = 0.69 ± 0.07 )Hot spot location was changed?
11Energy Release in the X-ray Outbursts
e
r
u
t
a
Fe

2.

2

Thermal X-rays

Hard X-ray

Heat conduction to the surface
Formation of hotspot

4.
Accelerated particle

e
r
u
t
a
Fe

Magnetosphere

Magnetar
e
n
g
a

1

Short Burst

ield
F
tic

M

1.
Deformation of Magnetosphere
Starquake in magnetar crust
3
e
r
u
t
Glitch-like behaviorFea

Reconnection

Magnetic Energy

Fireball

Thermal Energy

3.

Short Bursts(Note) Photon splitting effect to produce the hard X-rays?
Hot spot produced by injection of accelerated particles?
12

Broadband X-ray Spectra vs. Magnetic Field
Suzaku performed “Magnetar Key Project” anddetected the “hard X-ray component” from ~7 magnetars.
Hard

High-B, Young

SGR
1806-20 (2.1x10(0.22 kyr)11 T)
SGR 1806-20
10 T)
1E1E
1547.0-5408(1.4 kyr)1547-54 (2.2x10
10 T)
1RXS
J1708-40 (4.7x10(9.0
1RXS
J170849.0-400910
kyr)
10
4U 0142+61
0142+61 (1.3x10
4U(70 kyr) T)(Enoto+2010)

1

10+DUGQHVV5DWLRȟ /h/s

2
-2 -1
-1
keV
(ph
cm
s
keV
)
2 cm-2 sec-1 keV-1 (a.u.)
keVnormalized
at 2 keV

ThermalLow-B, Old

High-B, Young

10

1900+140501+45(2009)

1

0.1

1806-201547-540501+45

1841-04(2008)

1708-40

2259+58
0142+61(Enoto+2010,
Astro. Phys. Lett.)

Low-B, Old

Energy (keV)

100

1010
1011
Magnetic Field (G)Luminosity of the hard X-ray component is found to be positively correlatedwith their magnetic field derived by Period P and its derivative Pdot.
2 Types of Magnetars (SGR & AXP) show broad-band X-ray spectral evolution !
One key feature of the hard X-ray emission mechanism.
13Diversity of Neutron Stars
Fast Spin-down

Broad-band X-ray spectral
Magnetars

evolution with B and age. (TE+10)1014

QED Critical Field
4.4x1013 G

Young
1013

Binary X-ray
Pulsar (B<7.5x1012 G)
SGR 0418+5729

Crab-like pulsar

Magnetar-like outburst
Rea+10, Science1012 G

1012
1011

em

iss

io

n

Radio pulsar

Magnetar Descendant
old and X-ray quiet, but
Old sometimes activates to outbursts

dioHiddennew large population !
1010

ms pulsar

109

d

of

ra

Rotation-powered
Accretion-powered
Magnetically-powered
Magnetically-powered

En

Surface Magnetic Field (Gauss)

Birth!!

X-ray burster
0.001

0.01

0.1

1

10

100

1000

Rotation Period (sec)Toroidal Field
Braithwaite+09

14

Signatures of Toroidal Field: Low-B Magnetar• Low-Bd magnetars (Bd < 3.3x1013 G): SGR 0418+5729 and Swift J1822.3-1606• Magnetar burst activity requires high-B field than measured Bd~6x1012 G.
• Short-burst originates from reconnection? Higher multipoles?
• Discovery of proton(?) cyclotron signature in SGR 0418+5729• Strong multiple signature with B>2x1014 G near the NS surface• Simulations of the toroidal field inside the NS (e.g., wound-up at the birth)

Energy source of magnetars = Poloidal + “Toroidal” Magnetic field ?
Multipole?
Poloidal

SGR 0418+5729

P-Pdot observations

Tiengo et al., 2013, Nature(C) ESA

Toroidal??
1

2

5Energy (keV)

Difficult to measure
Braithwaite+09
15

Psoft = 8.68891 ± 0.00010 sec(1)

2

Zn /2n (16 bins)
Reduced chisquare

Reduced chisquarewith whereinpossible thestructurs[19], we
tried
n=
tion,
hard X-ray
pulseswere150
As0142+61
presented in Fig. 1 (b), the HXD pe
Soft
and
Hard
X-ray
Pulsation:
4U
ich agrees with previous measurements of the periodn = 3 and 4 both show a small peak100
this source and its derivative [20]. The folded
soft
(a)
14
withintheanderror
range
of ~100
eq.(1),
but i
Famous and prototypical AXP: Bd~1.3x10 G. Observedin 2007
2009
(both
ksec)
ay pulse
50 profile is shown in Fig. 2 (a).
rather low,20and higher peaks are seen
Pulse
profileP
ods.
(The case withRotationn = 2axis
is similar.) Th
soft = 8.68891±0.00010 sec
250
15
0.4-4 keV
expected,asthe hard X-ray intensity aSoft 0.4-10 keV
3.0 (b)(a) XIS
HXD-PIN
Magnetic
axisin t
200
time
were
both
very
similartothose
n=3 n=410
2.5
tion, wherein the hard X-ray pulses were
150
2.0
5
4-10 keV
1.5

100

0

1.0
50

0.31
20

0

2

15

5
0

8.687

8.688

8.689

Period (sec)

8.690

0.29
10

0.28
5

0.27
0

Hard Power-law
Soft thermal(b)0.31 (c) Magnetosphere
Hot spot 0.31

10

1.0
0.5

0.30
15

0.26

8.691
35

X-ray Intensity (c/s)

4

Zn /2n Z 2 /8

25
20

1.5
2.0
1.0

00

30

2

2.0
3.0

35

Z4

Hard 15-40 keV(b) HXD-PIN
4.0(c) HXD-PIN
n=3 n=4
2.5(demodulated)
3.0

X-ray Intensity (c/s)

0.5

(a)
(b)

(or magnetic multipole)

0.30
0.30
0.29
0.29

2

Z4 /8

2

Z4

(c) HXD-PIN
30(demodulated)
0.28
8.69
sec
pulsation
signal
was
weak
in
hard
X-raysinthe2009 observation.
0.28
25
G. 1: (a)3.0A 1–10 keV XIS periodogram, calculated via stan0.27
d folding analysis using 16 phase bins per cycle. 20Data from
0.27Makishima & Enoto et al., submitted
2.0 and XIS3 were co-added, without removing
16
S0, XIS1,
back15
4.0

Reduced chisquare (16 bins)

being > 0.30 for each data set). Thus, we can rule outof this source and its derivative [20]. The fol
X-ray pulse profile is shown in Fig. 2 (a).
Phase
anySlow
instrumental
originModulation?
for the 55 ksec pulse-phase mod250
ulation in 4U 0142+61. We next re-analyzed the 2007

Assuming △t = A sin(2π t/T-φ) and search A, T, φA

Z42 at T=55 ks(a) XIS

200
150
100
50

before3.0

n=3 n=4

2.0

2

Zn /2n2.5(b) HXD-PIN

1.5
1.0
0.5

4.0

2

Z4 /8

0

(c) HXD-PIN(demodulated)

3.0

35
30
25
20

2.0

1.0

15
10
5

φ

T

after demodulation
0
8.687
8.688
8.689
8.690
Period (sec)with A, T, and φ

0

8.691

FIG. 1: (a) A 1–10 keV XIS periodogram, calculated
folding analysis
bins perHard X-ray (15-40 keV)shows phase modulation dard
by A=0.7
sec using
with16 aphaseT~1.5
h.cycle. D
2
XIS0, XIS1, and XIS3 were co-added, without remov
FIG. 3: Results of the Z4 “demodulation” analysis, obtained
ground. (b) Periodograms
theetbackground-incl
Makishima &from
Enotoal., submitted
by assuming a periodic phase shift in the 15–40 keV HXD
40 HXD-PIN data, calculated using the Zn2 techni
17Interpretation of the Slow Phase Modulation• Statistically significant?: YES• Chance probability (Z42=39.2) ~ 4x10-6. (Z2, Z3, and Z4 gave consistent results)• Instrumental effect or noise?: NO• Blank-sky data and bright Crab Nebula: Z42 <30• Doppler effect of a hidden binary companion? : NO
• observed T and A gives Mc~0.12Msun/sin i >~ 0.1Msun• Inconsistent with pulsed optical properties (likely to emerge from a NS)• Free Precession of Isolated NS??
Poloidal• Poloidal field Bd• can be measured from P and Pdot
• makes a star the “oblate” shape
Toroidal• Toroidal field Bt• can not be measured from P and Pdot
• makes a star the “prolate” shape

=

I
I

k

10 4

Bt
1016 G2

k=4~9 (Determined by EoS), e.g., Gualtieri et al., 2011

Braithwaite,
2009, MNRAS

NS with strong Bt is deformed into a prolate shape with ε~10-3~-4
Makishima & Enoto et al., submitted
18

Free Precession of Axisymmetric Rigid Body
Three vectors and two angles
Angularmomentum L

Axis of symmetry(dipolar magnetic axis)

P1=2πI1/L

α

Maximum photon
emissivitiyγ

Slowly rotate aroundaxis of symmetry
with a “slip period” Q

Q=(C) http://faculty.ifmo.ru/butikov/Applets/Precession.html

See. e.g.,
Landau and Lifshitz,
Mechanics

P1

=

1
P3

1
P1

1

Pulse-phase modulation become detectable when the NS is axisymmetric (ε≠0)
and has a finite wobbling angle (α≠0), and its emission peak direction is deviatedfrom the symmetry axis (γ≠0). [asymmetry ε]=[Spin period P]/[slip period Q]
Makishima & Enoto et al., submitted
19

Evidence on the Toroidal Magnetic Field
Rotation period

Phard
P1
=
=
Q
T
Slip period

1.6

10 4

Phase modulation

=

I
I

k

10 4

Bt
1016 G2

k=4~9 (Determined by EoS)

Observational evidence for toroidal field, Bt~1015-16 G, inside the NS.
• Why 4U 0142+61 shows such a signature?
•

Two components (Soft and Hard X-rays) is effectively used to detect the signature.

•γ≠0 is fulfilled. B-field configulation (multipole component) may wander around on the star.

• Comparing other types of X-ray pulsars?
•

Accretion-powered: forced precession•

Fast-rotating: centrifugal force makes the NS oblate and precession would be damped.

Evidence for the toroidal magnetic field is suggested by the Suzaku observation.
Makishima & Enoto et al., submitted
20

Diversity of Neutron Stars
Magnetars in Binary Systems?

Fast Spin-down

Magnetars

1014

QED Critical Field
4.4x1013 G

Young
1013

Binary X-ray Pulsar

Crab-like pulsar

1012 G

1012
1011

em

iss

io

n

Radio pulsar

Magnetar Descendant
old and X-ray quiet, but
Old sometimes activates to outbursts

dioHiddennew large population !
1010

ms pulsar

109

d

of

ra

Rotation-powered
Accretion-powered
Magnetically-powered
Magnetically-powered

En

Surface Magnetic Field (Gauss)

Birth!!

X-ray burster
0.001

0.01

0.1

1

10

100

1000

Rotation
Period(sec)
Toroidal Field does exists!!

Toroidal Field
Braithwaite+09

21

X-ray Intensity (mCrab)

X-ray Intensity (mCrab)smaller mass-loss rate (! 10up and down. This also suggests that the NS−1terminal
velocity(!100
kms
lly slowing
down
duringat
12 low accretion-rate
ENOTO
ET AL.
Magnetars
in
X-ray
Binaries?
If following the stellar evolution
hile enter a spin-up trend correlated to high aclicity M4-5 III star has 1.2 M"
tes •during
Therefore,
it isBinaries
reasonable
Longoutbursts.
Period Pulsars
in X-ray(Mattana et al. 2006), an escap
e the source
to be
near
equilibrium
period of• P~1.6
hour(IGRanJ16358-4726;
Patel+2007)−1
momentumtransfer.
panion
star
is
slow
∼
76
km
s
• P~1.6 hour (4U 2206+54; Reig+2002)
wing the• standard
disc accretion model (Ghoshthe present consensus of the wiP~2.7 hour (4U 0114+65; Li+1999)−11979), theequilibrium
periodat(Shakura
et
al.
least
a
few
hundredkms, usi• P~5.4 hour (4U 1954+319; Corbet+2008)
written as
on the velocity at ∼100–200 km• Standard accretion theory (Gosh & Lamb 1979)Oph(acompanion
of
the
SyX
6/7
−3/7
• Peq ≈ 7µ30 Ṁ16
B~1014-16 G?
s,(4)
et al. 1998; Hinkle et al. 2006).
Figure 1. Distribution of NS rotation periods in HMXBs (Liu et al. 2006), LMXBs (Liu et al. 2007), andFigure 15 represents possib
16
−1
30
3
/(10 g s Or
) alternativeand µ30 =µ/(10G cm theory?
)
16 =ṀMagnetars?
new accretionṀ , and B) in Eq (5) to rea
ccretion rate and NS magnetic dipole moment,
Figure 1. Distribution of NS rotation periods
in HMXBs (Liu Lineet al. 2006),
LMXBs
4U1954+319.
aassumes2009
2009(Liu
2
1997 accretion
2000
2001 M162004
2008
2009
2012
ely. The observedrate= 0.352005
07
12
0
−1
300
km
s
and
the
orbitalpewith Peq70 # 19400 s (∼5.4 hour) gives the ex5.9 hMAX
MAXI
MAXI
the 2004
observedṀ162008=0.382009(the22
trig.1
trig.2
trig.1
16
1954+319(a) field365reaching
(b)
60
1997
2000
2001
2005
igh4U
magnetic
B
∼
10
G.
One
RXTE/ASM
Swift/BATdays
70
the same but for Ṁ16 =MAXI
0.047 (
in prep
ation is50a Enotomagnetaras pointed
out for SyXB(a) ave. 365 days
PulseaPeriod indicates that the P ∼ trig.1
5.4
hou
60 running58−4726(Pateletal.
2007).
However,such
40
can be explained in the magnet
50 than that of thene order30 of magnitude higher
5.4
h
15
c,
d,
e,
and
f
represent
possib40
field of a magnetar SGR 1806-20 (2.4 × 10
20
Eq (5). Even though unknown
30
es, there
is no evidence on magnetar
activities,
10
large acceptable range of B, th
20 González-Galánhort bursts
and giant flares. As
becomes much weaker than the012) argued
that the spin and 10
X-ray intensity be-10

0

51000

52000
-10

53000
51000

54000
52000

55000
53000

4.9 h

56000 55000
54000 MJD (day)
55000

22M

Suzaku observation of a symbiotic X-ray bin
16••

Observational Property with Suzaku
1. Slowest spin period P~5.4 hour
2. High pulsed fraction 50-90%
3. ~100 sec shot-like burst
4. Hard X-ray spectrum
Magnetars?

3

ENOTO ET AL.

12

Enoto in prep

(a)

2012

0.11

0.010

2011

3

(b) 2011 quiescent

10−3
2

10−4

No burst activity

1

Quasi-spherical accretion (Shakura+2010)?
ENOTO ET AL.

Bow
sh

10−5
4
20
0
80
−2
−4
60
4
2
40
0
−2
20
−4

χ
χ
Count Rate (cnt s-1)•

keV2 (Photons cm−2 s−1 keV−1)
Count Rate (cnt s-1)
Count Rate (cnt s-1)

Slowest Rotating X-ray Pulsar 4U 1954+319(a) 2011 quiescent

ock

(c)

(b)

2012 flare

(c)
1

10

0

Vw

80

(d)

40
20
0

Ratio

0

RA

RB

2.4
2.2
2
1.8
1.6
1.4
1.2
1
0.8
0.6
2.4
2.2
2
1.8
1.6
1.4
1.2
1
0.8
0.6
2.4
2.2
2
1.8
1.6
1.4
1.2
1
0.8
0.6

(a) 0.5-4.0 keV(b) 4.0-10.0 keV 1000
500

1500

2000

2500

Figure 4. Enlarged XIS 1–10 keV light curves of Figure 3(b) during the 2011 obse
Long spin pulsar~ 1012-13 G pulsar ?
is binned with 8 sec.
(c) 15.0-70.0 keV
Ratio

Quasi-sphericalshell

2012 flare

60

Ratio

M-typeCount Rate (cnt s-1)

Figure 10. (a) X-ray spectra of 4U1954+319 in νFν form observed in 2011 quiescent and 2012 flare-up observation
continuum (Model C). (b) Residual of the comptt model in 2012. (c) the same as panel b but in 2011.

Enoto to be submitted(d) 4-10 keV/0.5-4 keV

23

Next X-ray Observatory: ASTRO-H

Two Priority Targets (Case-study Examples)
Broad-band and high resolution spectroscopy: Japan-US collaboration
1E 1841-045 & Kes 73
1E 2259+586 & CTB 109
No. 1, 2004

S
SX

V
Fo

(3’

)

Magnetar
AXP 1E 1841-045

SXT HPD
radius 0.65’

Fo
I
SX

’

325

CTB 109

SXI (19’)

Kes 739
1
V

XMM-NEWTON OBSERVATIONS OF CTB 109

SXS FoV (3’)

Magnetar
AXP 1E 2259+586

Fig. 2.—Mosaic RGB image created from EPIC data of the pointings E, N, S, and P2 obtained in full frame and extended full frame mode: R ¼ 0:3 0:9 keV,
G ¼ 0:9 1:5 keV, B ¼ 1:5 4:0 keV. The image is smoothed (see x 2.1).

•••

1.1 above
2.4 two targets
20.2
40.7
0.5
81.3
are
potentially
nice
to of
challenge
the fiveThequestions.
Figure20:The(left)The
SNR5.0Kes 7310.1
with
Chandrawith candidates
the
SXS162.0fieldview overlaid.
central source is the
Broad-band(0.2-600
withsensitivities.
AXP 1E
1841–045.keV)(right)spectroscopy
The SNR CTB 109
withhigh
XMM-Newton(Sasaki et al., 2004) with ASTRO-H SXS andandsomepossibleinterestingtargets;
SXI fieldof views. The
centralsourceisthesoft
AXPX-ray
1E 2259+586.
The
dim halfcalorimeter.
part of this SNR is covered by aHigh energy
resolution
(a
few
eV)
in
the
band
using
1RXS J1708-4009, and SGR 1806-20, Anti-magnetarthe
Puppis A’s CCO (?)
giant molecular cloud.
0.0

0.2

smoothed with a circular Gaussian function that has a sigmaof 3 pixels in both right ascension and declination. In the 4.0–
12.0 keV images, only significant emission from the pulsar isseen, but not from the rest of the SNR.
Figure 1 shows a mosaic image in the energy band of 0.3–
4.0 keV in false color. The remnant’s X-ray emission fades off
to the west, lacking a clearly defined edge. In the interior, theLobe is brighter than any part of the shell and there are dark
regions north and south of the Lobe. The Lobe emission is well
separated from the pulsar. We estimate the distance of the shellfrom the pulsar in the mosaic image by fitting a circle centeredon the pulsar to each sector and obtain 18A5 for the easternshell, 17A3 for the southern shell, and 16A6 for the northernshell. Thus, the eastern shell has the largest projected distancefrom the pulsar.

below 4 keV in order to identify possible spectral variations
within the remnant. The images in the red (R ¼ 0:3 0:9 keV ),green (G ¼ 0:9 1:5 keV), and blue (B ¼ 1:5 4:0 keV ) bands
are combined into an RGB mosaic image ( Fig. 2). We then use
this image to guide our selection of regions to be examined moreclosely through detailed spectral fitting. The selected regions
are shown in Figure 3.
The shell is slightly redder than the interior and has some redclumps. There is a small sector of the shell with lower emission
in the northeast, coinciding with a bright region in the radio
continuum (Kothes et al. 2002). Next to this region, there are
red knots in the RGB composite image of the X-ray shell (regions 5 and 6 in Fig. 3). Furthermore, there is a larger red spot 2
in the south (region 15). There are also color variations within
the Lobe, the outskirts being redder than the central part of theLobe.
In addition to the very bright pulsar, fainter point sources
are found in and around the remnant. Two point sources located southeast of the remnant appear red in the RGB composite

Science challenges towards NSs and magnetars• Search for proton cyclotron from magnetars and determine the B field.
energy ∼0.75 keV (hereafter emission) or as a cyclotron absorption feature plus a harmonic• Study of NS and magnetar atmosphere models
with an energy of E0 ∼0.46 keV, hereafter cyclotron (Gotthelf et al., 2013). It wasn’t possible• Precisemeasurements
ofthesesupernova
remnantof magnetars:
Their birth
to distinguishbetweenmodels using
Chandraand XMM-Newton
data.environment• Hard X-ray
power-lawtheirtheoriginrelated
withSXS
QED
physics.
In Figure
18, weandillustratecapabilityof thein differentiating
between the emission
model and the cyclotron model using a 100 ksec exposure. This particular CCO was selected24based on its location near the centre of a large and not so bright SNR (in comparison for2.2. RGB Composite Imagge

As no emission from the remnant is found above 4 keV
except from the pulsar, we create images in the energy bands

ASCA, Suzaku, and other missions, NICER’s XRCs are not imaging optics — Xction. Neutron
The absence ofstar
secondarymirrors Composition
increases efficiency anddecreases mass(NICER)
andInterior
ExploreR
optical system that is optimized for observations of point sources. NICER’s optical
Approved as a NASA Explorer Mission of Opportunity
al bench, is provided by NASA GSFC.

Gendreau, Arzoumanian, and Okajima et al. 2012, SPIE

peak
X-ray
collecting
exceeds
that
XMM-Newton’s• effective
Soft X-ray(0.2-12keV)area
timing(<300
nsofreso.)
spectroscopy with a large effective areamorea factor ofoftwo.
• than56 modules
Grazing-incidence optics coupled with silicon drift detectors••

Payload to the International Space Station (ISS) in 2016
High precision measurement of NS Mass and Radius: the EoS and NS interior•

Phase-resolved spectroscopy method of NS hot spots, Shapiro delay in X-rays
25

Summary• Recent discoveries of transient magnetars have increased numberof the “magnetar” class.

• The non-thermal hard X-ray component was discovered both inpersistent magnetars and transient sources.Relative luminosity
between soft and hard X-ray components shows spectral evolution
as a function of the magnetic field and age.

• 1.5-hour phase modulation was detected. This is interpreted as afree precession due to toroidal magnetic field embedded in themagnetar interior.

• Long period pulsars were recently discovered in X-ray binaries.
These become magnetars if following to the standard accretion
theory, but can be regarded as 1012-13 G pulsars if different
accretion model are assumed.

26