連星⽩⾊矮星合体とその後の進化について
樫⼭和⼰（東⼤理）

double WD merger remnant

Highly magnetizedmassive white dwarf?
WD pulsar? …

Type Ia
supernova?

Collapse into
neutron star?
GRB? FRB?
…

a circular mid-infrared nebula. The widths
ply that wind material leaves the star with
6,000 kilometres per second and that rapid
ong magnetic field aid the wind acceleration.
d helium are probably absent from the starde that both objects formed recently fromsive white dwarfs. Our stellar-atmosphereate a stellar surface temperature of aboutminosity of about 104.6 solar luminosities.
tar and nebula agree with models of then of super-Chandrasekhar-mass whitea bright optical and high-energy transient
r11 within the next few thousand years. Ourat super-Chandrasekhar-mass white-dwarf
monuclear explosion as type Ia supernovae,
the generation of magnetic fields in stellar

ions. The lines may either originate from a hot plasma that coexists withthe cooler simulated wind material in our models, or indicate a highneon abundance (see Methods). Our model fit yields a stellar temper40,000
ature of 211, 000−+23,000
K (see footnote of Table 1 for the definition of
the uncertainities) at the base of the wind and a chemical composition

Gvaramadze et al.19

A pale blue dot in
an infra nebula
WS35 (= J005311)

for mid-infrared circumstellar nebulae
covered a new object in the constellation
g data from the Wide-field Infrared Survey
wavelength of 22 µm the new nebula appears
agged edges and an angular radius of about
ntrast 22-µm image of the nebula shows a diff about 110 arcsec surrounding the shell. For
to the nebula (see below), the linear radii ofout 1.1 pc and 1.6 pc, respectively. The shell is
2-µm image, where it appears as a circular dife angular size as the 22-µm shell. Surprisingly,
tinction towards the nebula (see below), thenterpart in the INT Photometric Hα Survey
Galactic Plane13 (see Fig. 1). We identified the

a

b

N
E

2 arcmincdtly ? reported observation of an extremely
hot white dwarf (WD)
1. INTRODUCTION
TRODUCTION
Recently?indic
repo
we
call
this
objectWD
J005311.
The
spectroscopic
analysis
LETTERRESEARCH
The
pale
blue
dot
on
the
HR
diagramtly? reported
observationof an extremely
hot whitedwarfwe(WD)int whitedwarf (WD)in a mid-infrared
nebula J005311.
Inpaper,thiscall thisristics
can besummarized
as follows.spectroscopic analysis indicate
wecallanalysis
this
objectWDthe
J005311.
copic
indicates
existenceTheof a peculiar wind. characteristics
The
canthat its mass also exceeds
the Chand+40,000
ristics
can besummarizedofas
follows.
e eﬀective
temperature
WD
J005311 is Tperspective
that000
it will−23,000
produce aK.
low
eﬀ = 211,•
Theeﬀective
10 R
10 R
10 R
10 R
future, accompanied
by a high-ener
4.8+40,000+40,000
11
supernova
211, 000−23,000
K. J005311
eﬀectivetemperatureof WD
is Teﬀ= and
211,.the000−23,000K.
ee=distanceto WD
is dJ005311= 3.07+0.34
kpc
bolometric
−0.28
• two
The
The merging ofstarsdistancein a binary
10% of the massive main-sequence s
4.6
+0.34
0eand
±
0.14.
4.60 ± 0.14.
the bolometriciscalculated
as
log(L
/Lthe
) =bolometricdistance
to WD luminosity
J005311
is
d
=
3.07
kpc
and
lu
⊙white−0.28
theradknown
dwarfs26, are thou
~1 kyr2very unusual wind of J005311 strong
0.14.
3
The R
photospe0 ±photosphericradiusis estimated to be r = 0.15 ±•0.04
.
4.4
0

1

2

3

~5 kyr~10log(L/L )kyrphmergers can indeed produce⊙highly
explain the magnetic stars of the upp=e0.15± 0.04 R⊙ . radius is estimated to be rph =photospheric
0.15ofby± 0.04R⊙dwarfs.and24.ox•ThechemicamationmagneticwhiteOue chemicalcomposition
of
the
wind
is
dominatedcarbon4.2
the ongoing debate on whether a sup
4
tedbycarbonandoxygen
(X
=
0.2
±
0.1
and
X
=
0.8by
± 0.1).
Cthe wind
O of twocarbon–oxygen
white
dwarfsee chemicalcompositionofisdominatedcarbon
and
oxyg
•
The
neon
ma
1
neon
mass
fraction
(X
=
0.01)
is
significantly
largerthan
theNe
which J005311 appears to provide a c
4.0
fraction(XtoFe−3
themergermass
producedenough heat
ntly
larger
than
the
solar
abundance
while
the
iron
group
ction
(X
=
1.6
×
10
)
is
consistent
with
that.
e neon mass
Fe fraction (XNe = 0.01) is significantly larger than the sol
to ignite carbon non-explosively. The s
–1R
at.
−3
4.8
10
• Fromthe wid
ing stages was thus
only interrupted
ction (XFe = 1.6 × 10 ) Gvaramadze
is consistent
with
that.
al.19
om the width and strength of theet O
lines, theVI emission
both components
andvistermina
now
expec
as
=
16,
0
∞
Schwabet al. 16nlines,
theterminal
velocity
andmass-loss
rate
areestimated
−1
−6
−1
core
collapsewithin
the
next
few
tho
3.6 16,v∞ the=000 ±1, 000km s of andṀVI=emission(3.5 ±
0.6)
× 10
M
yr
om
width
and
strengththe Olines,
thelarger
terminal
vbt
⊙than
−6
−1
produceaneutrino
flash
and
a
γ
-ray
0.6) × 10 M⊙ yr , respectively.
Note that v∞ is significantly−6 Ic supernova
−1
11
type
ger
than
escapeatthephotosphericradius,
v
(r
v∞ =
16,
000 5.0±
1, 0004.5velocity
km s−1
Ṁ
(3.5
0.6)
×
10
M
yr
,. )re∼5.5 the
4.0 and3.5 =3.0 ± subluminous
esc
ph
⊙
−1

ric radius, vesc (rph ) ∼ 1,log[T600(K)]km s .
•vThe(rapparen
ger than the escape velocity
at the photosphericradius,Online content esc ph ) ∼ 1
effneported
this paper,
we call thisWD J005311.
spectroscopic
analysisindicamechanism
and Thefateof the
wind
mass
loss.
observationof anobject
extremely
hot1.white
dwarf
(WD)
in
a
mid-infrared
INTRODUCTION
hecharacteristics
canbesummarizedasfollows.
In
Gvaramadze
et al.indicates(2019), theauthors ass
this object WD J005311. The spectroscopic analysis
the existenceof+40,000
Recently?
reported
observation
argue
that
the
terminal
velocity
of of
thean
reported
observation
of an
hot
white
dwarf (WD)inwind
aext
mic
of WD
J005311is Textremely
=
211,
000
ntemperature
be summarized
as follows.
∗−23,000 K.
8magnetic
field
of
B
∼
10
G and
the wind accell this object WD J005311.
The
spectroscopic
analysisindicatesthepaper,
wecall
this
objectWD
J005311.
Th∗+40,000+0.34
J005311
is
T
=
211,
000
K.
∗
to WD J005311
is d = 3.07
pc andthis
thepicturebolometricluminosity
is calculate−23,000−0.28
However,may
haveadrawback.
Gvaramadze
et al.19If
csRESEARCH
can LETTER
be summarizedasfollows.
characteristics can be summarized as follows
profile would be detected. But
emissiond = 3.07+0.34
asthe
log(L
=
+40,000∗ /L⊙ ) lin−0.28 pc and the bolometric luminosity is calculated
ective temperature of WD
J005311
is
T
=
211,
000
K.
eﬀ temperature
The
of WD
J0053
key
wind,
e.g., thelauheric radius is estimated to •beOtherR∗ =eﬀective
0.15 components± 0.04R⊙ . of the−23,000
1
+0.34
To
this
end,kpc
here
wethe
constructa consistentw
stancetoWD
J005311
is
d
=
3.07
and
bolometricluminos
composition
of
the
wind
is
dominatedbycarbonandoxygen
(X
=
0.2
±
0.1
an
−0.28
ated to be R∗ = 0.15 ± 0.04 •R⊙The.
C is d = 3.0
distance
to WD
J005311ourmodel,
the
base
of
the
wind
is
the surface o
0.14.
dth
strength ofby
the
OVI emission
lines,
themass-loss
4.60
±
0.14.
windandis dominatedcarbonandoxygen(X
0.2wind.
± 0.1velocity
and XOand= 0.8± 0.1).
oftheWD
J005311C =terminal−1−6−100 ± 1, 000 kms andṀ = (3.5 ± to0.6)be× r10
M0.15
respectively.
Note that⊙ yr ±, 0.04
otosphericradiusis estimated
R⊙ .
ph =
the
OVI emission
velocity
mass-loss
rate
are=estimated• The
neon andmass
fraction
(X
0.01)
is ts
•terminalThe
photosphericradiusiskm
estimatedNe
he escapevelocity lines,
at thethephotosphericradius,whichis∼ 1, 600
s−1
.
−6
−1
nd
Ṁ =composition(3.5 ± 0.6) × 10
M⊙windyr fraction,isrespectively.
that
∞and
emicalof thedominatedcarbonoxygen (X(XFe Note=by1.6× 10v−3)isissignificantly
consistent−1which corresponds to rnb ∼
tthe
size
of the infrared nebulais∆θ
∼1, 10is ∼chemical
600arcmin,km scomposition.
•Theof the wind i
0 photospheric radius, which−1locityof vnb∼ 100 kmage chemicalofnebulais estimatedto bethe∼consistent
16,
000ab
yr
The
abundanceis broadly
on mass
fraction(XsNe ,=the0.01)
is thesignificantly
largerthan
solar
nebulais1.6∆θ×∼1010
whichcorresponds
to 7500
rnbrealized∼ 0.01
pc.
From
thei
−3arcmin,
3500
4000
4500
5000
5500
6000
6500
7000
Similarsituation
can
be
in
the
merger
•
The
neon
mass
fraction(X=
0.01)
nd(2019)(X=)
isconsistent
with
that.
Ne
Fe
proposed that WD J005311
is a super-Chandrasekhar-mass remnant ofoλ[A ]m s−1 , the age of the nebula ismerged
estimated
toWD,
be ∼the16,oﬀ-center
000 yr. −3carbon ignition
CO
te
dwarf
theof models
observed
and
L
and
the
absenceof hydrogenafraction(X=
1.6
×(blue)10 terminal) isconsisten
Extended
Data Fig. 1 merger,| Neon features in ourgiven
models. Comparison
with neon surfaceT
massfractionsof
0.0(red),
0.1(green)and
0.5∗
Fe ∗ lines,
with observations(black).and
The observedstrengthand calculated fluxes are dividedbythe same O
modelled continuum
flux f .
he
width
of
the
emissionthevelocitreachesVIthe center,remnant
the Kelvin-Helmholtz
contraat WD J005311 is a super-Chandrasekhar-massof double degenerate
−1
−6
−1
= 16,
± 1, 000Ṁ(3.5±of0.6)× 10
M⊙
yr of, broadly
respect
From
the
width
and
strengththeO
ven
the000observedT∗km
ands L∗•and
and
the =
absencehydrogenandheliumoccur.
We
regardthesecarbonburning
is respo: Kazumi
Kashiyama
Line
width
& height
thantheescapevelocity atasthephotosphericradius,vesc(r)model∼and
1, 600−1phAnother
importantfeature
of
our
is
v
=
16,
000
±
1,
000
km
s
Ṁt
∞
okyo.ac.jp
acceleration
the escaperotating velocity
magnetic fieldoccu
larger thanbytheat the
p
O VI

C IV

Ne VIIIOVNe VIII

C IV

OV

O VI

C IV

O VI

Ne VIII

Ne VII

Ne VIIlog f λ /f c

O VI

Ne enriched C/O dominated windc!?

ing and highly magnetized central star with The line spectrum is reproduce
00 years9,10. Here we report observationsof lines
near 4,340
Å andwith
6,068 ÅA white dwarf
mergerproduct
um dominated by emission lines, which is lying transitions of highly ion
a super-Chandrasekhar
a circular mid-infrared nebula. The
widths ions. The lines maymass
either origin
Gvaramadze
et al.19
mply that wind material leaves the star with the cooler simulated
wind
ma
6,000 kilometres per second and that rapid neon abundance (see Methods
40,000
ong magnetic field aid the wind acceleration. ature of 211, 000−+23,000
K (see fnd helium are probably absent from the star the uncertainities) at the base ode that both objects formed recently from~10tsiveimwhite dwarfs. Our stellar-atmospherekyrcate aestellar surface temperature of aboutaminosity of about 104.6 solar luminosities.
star and nebula agree with models of theon of super-Chandrasekhar-mass whitea bright optical and high-energy transient
r11 within the next few thousand years. Our
hat super-Chandrasekhar-mass white-dwarf
monuclear explosion as type Ia supernovae,
f the generation of magnetic fields in stellar
RESEARCH LETTER

100R

4.8

101R

4.6

102R

~1 kyr2

3~5 kyr~1log(L/L )

0

ky
r

4.4

103R

4.2

4

1

4.0

10–1R

4.8

3.6

5.5

5.0

4.5
4.0
log[Teff (K)]

3.5

3.0

Fig. 3 | Position of J005311 in the Hertzsprung–Russell diagram. The
red cross marks the position of J005311, with error bars (see Table 1). Thisthat its mass also exceeds the Chandrasekhar limit, with the exciting
perspective that it will produce a low-mass neutron star in the near
future, accompanied by a high-energy transient and a fast-evolving
supernova11.
The merging of two stars in a binary system is not a rare event. About
10% of the massive main-sequence stars25, and a similar fraction of
the known white dwarfs26, are thought to be merger products. Thevery unusual wind of J005311 strongly supports the idea that stellar
mergers can indeed produce highly magnetized stars, which would
explain the magnetic stars of the upper main sequence27 and the formation of magnetic white dwarfs24. Our results may also help to resolve
the ongoing debate on whether a super-Chandrasekhar-mass mergerof two carbon–oxygen white dwarfs leads to a type Ia supernova, forwhich J005311 appears to provide a counter-example, indicating thatthe merger produced enough heat to prevent immediate collapse andto ignite carbon non-explosively. The sequence of thermonuclear burning stages was thus only interrupted during the white-dwarf stage ofboth components and is now expected to continue and to end in acore collapse within the next few thousand years9. This will probably
produce a neutrino flash and a γ-ray burst28, followed by a very fast andsubluminous type Ic supernova11.

Online content

Any methods, additional references, Nature Research reporting summaries, sourceed nebula. The widths
ial leaves the star withsecond and that rapid
d the wind acceleration.
ly absent from the star
formed recently fromur stellar-atmospheretemperature of about
04.6 solar luminosities.
ee with models of theasekhar-mass
white
tim
high-energy
transientew thousand years. Our
khar-mass white-dwarf
RESEARCH LETTERastype Ia supernovae,
agnetic fields in stellar
100R

4.8

101R

102R

103R

rcumstellar nebulae
t in the constellation
e-field Infrared Survey
he new nebula appears
ngular radius of about
the nebula shows a dif4.6~1 kyr2

3~5 kyr~1log(L/L )

0

ky
r

4.4

4.2

4

1

4.0

10–1R

4.8

3.6

5.5

5.0

4.5
4.0
log[Teff (K)]

3.5

3.0

Fig. 3 | Position of J005311 in the Hertzsprung–Russell diagram. The
red cross marks the position of J005311, with error bars (see Table 1). This

ions. The lines may either originate from a hot plasma that coexist
the cooler simulated wind material in our models, or indicate
will finally collapse into a neutron starneon abundance (see Methods). Our model fit yields a stellar te
40,000ature of 211, 000−+23,000
K (see footnote of Table 1 for the definit
Gvaramadze et al.19
the uncertainities) at the base of the wind and a chemical compo
a

~1
0

ky
r

b
E

af
ew
that its mass also exceeds the Chandrasekhar limit, with the exciting
perspective that it will produce a low-mass neutron star in the near
future, accompanied by a high-energy transient and a fast-evolving
supernova11.
The merging of two stars in a binary system is not a rare event. About
10% of the massive main-sequence stars25, and a similar fraction of
the known white dwarfs26, are thought to be merger products. Thevery unusual wind of J005311 strongly supports the idea that stellar
mergers can indeed produce highly magnetized stars, which would
explain the magnetic stars of the upper main sequence27 and the formation of magnetic white dwarfs24. Our results may also help to resolve
the ongoing debate on whether a super-Chandrasekhar-mass mergerof two carbon–oxygen white dwarfs leads to a type Ia supernova, forwhich J005311 appears to provide a counter-example, indicating thatthe merger produced enough heat to prevent immediate collapse andto ignite carbon non-explosively. The sequence of thermonuclear burning stages was thus only interrupted during the white-dwarf stage ofboth components and is now expected to continue and to end in acore collapse within the next few thousand years9. This will probably
produce a neutrino flash and a γ-ray burst28, followed by a very fast andsubluminous type Ic supernova11.

c

Online content

Any methods, additional references, Nature Research reporting summaries, source

2 arcmindkyr

Gvaramadze et al.19
Photosphere= base of the wind

Alfvén pointM⇤ > Mchvr ⇡ v1<latexit sha1_base64="FdU3NvRNRVE2v4Wcn/BR+TOhi74=">AAACdXichVHLSsNAFD2N7/qKuhFECFZFXNQbERQXIrpxI/hqK6iEJI4azIskLWjxB/wBF7pRUBE/w40/4MJPEJcVunHhbRoQFfUOM3PmzD13zswYvm2FEdFzSmpobGpuaW1Lt3d0dnXLPb350CsGpsiZnu0Fm4YeCttyRS6yIlts+oHQHcMWBeNwsbZfKIkgtDx3IzryxY6j77vWnmXqEVOaLC9r48qcsqyVtwNHMQ9ONDlDWYpD+QnUBGSQxIon32Ibu/BgoggHAi4ixjZ0hNy2oILgM7eDMnMBIyveFzhBmrVFzhKcoTN7yOM+r7YS1uV1rWYYq00+xeYesFLBCD3RHVXoke7phd5/rVWOa9S8HPFs1LXC17pP+9er/6ocniMcfKr+9BxhDzOxV4u9+zFTu4VZ15eOzyrrs2sj5VG6olf2f0nP9MA3cEtv5vWqWDtHmj9A/f7cP0F+MqtSVl2dyswvJF/RigEMYYzfexrzWMIKcnxuCRe4xk2qKg1Kw9JoPVVKJZo+fAlp4gMdSI9l</latexit>

ONe
core

<latexit sha1_base64="dRl2VwsrgaBl6YfuRC+ncwumjCo=">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</latexit>B⇤ ⇠ 108 G

rph ⇠ 1010 cm<latexit sha1_base64="cm7kEfRkP58LU9Ag3sjOqLoPvQM=">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</latexit>rA ⇠ 1011 cm<latexit sha1_base64="DzhOM9ayESEmTjw0RnJtEdlo4Ok=">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</latexit>Kashiyama, Fujisawa, Shigeyama 19
Wind from WD J005311

Slow point

Alfvén point

3

Photosphere

Fast point

C burning

vr ⇠ 108 cm s 1

vr . v1 = a few ⇥ 109 cm s 1

vr ⇡ v1

ONecoreM⇤ = 1.1-1.3 M⌦ = 0.2-0.5 s 1

B⇤ = (2-5) ⇥ 107 G

rs ⇠ 109 cm

rA . rph ⇠ 1010 cm

Figure 1. Schematic picture of our wind model for white dwarf J005311.

rs & 1012 cm

arXiv:1907.12317

The launching mechanism• XC = 0.2, XO = 0.8, XNe = 0.1(but XFe = 1.6x10-3 similar to the solar abundance )<latexit sha1_base64="qvF6BWy5rvjWnZXgLq0+kC4pkH4=">AAACa3ichVHLSsNAFD2N7/qquhF1IZaKq3IjguJKdOOyrVYLbSlJHDWYJkOSFrX4Ay7duKgbBRHxM9z4Ay78BBFXCm5ceJMGREW9YTJnztxz58wdXVqm5xM9xJS29o7Oru6eeG9f/8BgYmh4w3NqriHyhmM5bkHXPGGZtsj7pm+JgnSFVtUtsanvrQT7m3XheqZjr/sHUpSr2o5tbpuG5jNVKGlSus5+vJJIUprCmPwJ1AgkEUXGSVyhhC04MFBDFQI2fMYWNHj8FaGCIJkro8Gcy8gM9wWOEGdtjbMEZ2jM7vF/h1fFiLV5HdT0QrXBp1g8XFZOIkX3dE0vdEc39Ejvv9ZqhDUCLwc86y2tkJXB49G1t39VVZ597H6q/vTsYxsLoVeTvcuQCW5htPT1w9OXtcVcqjFNF/TE/s/pgW75Bnb91bjMilwTwQOo39v9E2zMplVKq9m55NJy9BTdGMcUZrjf81jCKjLIh30+QRNnsWdlRBlTJlqpSizSjOBLKKkPF+WMxg==</latexit><latexit⇡
accretore.g.,
Truran & Livio 86
Hachisu & Kato 16“Neon novae”

ONe WDThe ONe mantle is dredged up

The launching mechanism• A similar situation can be realized on the surface ofa carbon/oxygen white dwarf merger remnant
Schwab et3465
al. 16
Super-Chandrasekhar WD merger remnants
In the merged CO WD, C is ignitedoff-center and the C-burning flame
propagates into the interior.

and now has a total mass of ≈1.3 M⊙ . The grey lines show the evolution ofa contracting 1.30 M⊙ pure neon model. Neon ignition does not occur andthe core instead becomes supported by electron degeneracy pressure. The
remnant will cool to form an ONe WD.

The timing is consistent with
the nebula age of J005311!

that it is difficult to produce an ONe core with a sufficient mass toundergo accretion-induced collapse (AIC) in a WD merger.

Downloaded from https://academic.oup.com/mn

The flame reaches the center in∼ 10 kyr after the merger,
neutrino cooling leads to the
Kelvin-Helmholtz contraction of
the ONe core and a series of offFigure 7. Same as Fig. 6, but for the version of model M15 with mass-loss
center C flashes occur.
during the cool giant phase (see Section 4). The remnant shed ≈0.2 M⊙

Weber & Davis 67
fast point
Alfven point

Slow point

The rotating magnetic windin the equatorial plainclassical Weber-Davis stellar wind solution (Weber & Davis 1eheWeber-Davisstellar(Weber& Davis&classicalHachisu1994).
As thefield
Weber-Davissolution only
concerns
thetoroidalmagnetic
Bφwindas solution
achisu 1994). As the Weber-Davis solution only concerns the w
ezing condition
with Faraday’s
law givestheconcerns
flux conserv
Hachisu1994). together
As the Weber-Davissolutiononly
theg condition
togetherwith field
Faraday’s
gives the flux conserv
2 Bφ as law
withthe toroidal
magneticng
condition
together
withFaraday’s
law
gives the flux conser
FB = r Br = const,
the toroidal magnetic field Bφ ash the toroidal magnetic field B2φ as

4 constraint equations
FB = r Br = const,

FB = r2 B
2 r = const,
vrφ =− const,
rΩ
FBB=
φ r B

=

BrBφ

.

vφv−
r rΩ
=
.
BφBr vφ − vrΩrrΩ
Bφ=of vthe
al and azimuthal velocity
respectively. The.
φ − wind,. respectively. The ma
Br =of thevr wind,radialandazimuthalvelocityBrvrs
bedandas azimuthal velocity of the wind,ial
respectively. The maṀ2dial and azimuthal velocity
ofr thewind,
respectively. The m
ρv
=
Ṁ
r
2
as
ρv
r
= 4π
r
as
Ṁ4π
!
"
2
Ṁ
ρvr r!rB
=
2 B "
rr4π
φφ
ρvr r rB=
B
L =L rv=
const,
4π= φrv−−=
const,
φ!
"
4πρv
4πρv
r
!rB B r "rBr r Bφφ = const,
L = rvφ −nsityof wind.
the wind.
The
betweengas
L=
rvφcoupling− 4πρv= theconst,of theThe
coupling
betweenthegasandandradiation
radiatir
4πρv

F
Br = const,
drB = r 16πacλT
r

2
dPg
κL
GMand
Bφ limiter.
dy, Lraddvisr the1radiation
luminosity,
We calcu
rad∗ λVisφ the flux
vr
+
−
+ 2 −
+
(rBφ ) = 0.
2
B
v
−
rΩ
sias &
Rogers1996),
assumingthemetalabundance
consistent
with tdr
ρ dr
4πr c φ r φr
4πρr dr=.
wing Levermore & PomraningB(1981).
The
vr momentum equation of the gar

3 evolution equations

dentical to the spherical radiation driven wind; the first, second, thirradialand azimuthal
velocity of
the wind,respectively.
The masaspressurepressure
gradient,
andgravitational2
dvr gradient,
1 dPg radiation
κLrad GM
V
B
d
∗
φ
φ
v
+
−
+
−
+
(rBφweight.
) = 0. Th
bedasby Pg r=drρkB Tρ /(µm
)
where
µ
is
the
mean
molecular
u
2
2
dr
4πr c
r
r
4πρr drṀ2celeration produced by the centrifugal
force and the magnetic slinρvr=re identical to the spherical radiation driven
4π wind; the first, second, third,tion
is given byn, gas pressure gradient, radiation!pressure"gradient, and gravitational ac!
"rB
Bφ mean molecular weight. The fi
rtheven by Pg = ρkB Tdε
/(µm
)
where
µ
is
= 1const,
d 1
dLrad
gL =u rvφ −4πρv=
vr+byPgthevr centrifugal− and,r forceacceleration produced
the magnetic
sling e2drdr ρ
4πr ρ drquationgiven
by The coupling between the gas and radiation is
nsity
of isthewind.
! ") is the gas energy
density.
Notethat
we neglect
theconvective
proximation,
wheredεthetemperature
gradient
canbedescribed
as l
d
1
1
dL
g
rad
+
P
v
=
−
, region and t
sts a convective vinterface
betweenthecarbonburningr
g r
2
drdr ρ κρLrad4πr ρ drdT
convective motion might beby ,strong magnetic fields.
= suppressed
−
3 r2
dr
16πacλT(6)(7)gascanbe transformedmis theenergydensity. Noteintothat we neglect the convective lumiu ) andexistsa convective
interface
betweenandthe carbon
region and$ radiation
Lluminosity,
flux
Wethe
ca
rad2 is2 the! λ is theburning" limiter.
A v

dεg
d 1
1 dLrad! "ux freezing
condition
together
withFaraday’s
law
gives, the flux conservation o
v
+
P
v
=
−
r
g
r
d 1
1 dLrad2 ρ dr
dr
dr
ρ
4πr
+tion
Pg vrwith the=toroidal−,(7)
field Bφ asdr ρ
4πr2 ρmagnetic
dr

3 evolution equations

εg = 3kB T /(2µmu ) is the gas energy density. Note that we neglect the convective luminosity in Eqs.
general,Notethere thatexistswea convective
interface
the=carbon
burning
FB between= r2 Bluminosity
const,
nsity.
neglect theconvective
in Eqs.region(6) andandthe wind region. Hrlso in our case, the convective motion might be suppressed by strong magnetic fields.
ace
between the carbon
region andinto
the wind region. However,
4 and (7)burningg Eqs. (1-4), Eqs. (6)can be transformed
Kashiyama et al. Kashiyama et al.
ight#be suppressed by strong
magnetic fields.
$"withBφ k vφ! −dTrΩ
2 2Av
ansformed
into
k
T
r
dv
κL
GM∗ Br2
Ar Aφ
B
r
rad
B
φ r
2
=
.
v
−
−
=
+
+
2T
−
+
v
+
2v
v
4 r
et al.
Arr = √ φ , r φ v 2 − A2 ,Br µmuKashiyamaµmu
vr2 − A2r vr dr
4πrc
dvB
log
r
r
4πρ
r
r
r
!
"

A4r = √
,
K
κL
k
dT
GM
A
A
rad
B
∗
r
φ
4πρ
being
the
radialAlfvénvelocity,
with2 the wind, respectively. The mass andre the+radial and azimuthal+ 2T −velocity+ vof,
φ + 2vr vφ 2Br
Bφ(8)
2
4πrc
µm
d
log
r
r
v
−
A
dε̄
κL
√
Ar = r, r Aφ = √
u
,
rad
with
described
asal Alfvénvelocity,
=
.
4πρ
4πρ
dr
4πr2B
cṀ
φ
2
√
A
=
,
being the azimuthal Alfvénvelocity,
andbeing the radial Alfvénvelocity,
ρvrφr =
4πρ
4π Bφ
dε̄
κLrad
A
= 1√ Alfvénvelocity,
, 2
being
the
Lradφradial
5 kT
2
!
"
=
.
(9)− GM∗ − rΩvφ +
4πρ
ε̄
=
+
(v
+
v
)
+
2
r
φ
muthaldr
Alfvénvelocity,
and
rBr B
Ṁφ 2 Kashiyama2 µm
4 4πr cet ual. r

L = rv= const,being the azimuthal Alfvénvelocity,andφ −
4πρv
Lrad In1total,2 we have
5 rkT equationsGM∗ (Eqs. 1-4) and 3 ordinary diﬀ
respectively.
2 4 constraint
ε̄ =
+
(v
+
v
)
+
−
− ∗rΩvφ + LΩ,
with 9)being
theazimuthalandLrrad
5 kT Alfvénvelocity,GM
2Lrad ).
for 7Ṁ
variables(ρ,vr ,+vφ1,φBT,
rr,2B+
φ ,2
2
µm
r
ε̄
=
(v
v
)
+
−
−
rΩv
+
LΩ, is treaBφφu the gas andass density of the wind. TheṀcoupling
between2
2 µmu Ar =r √ r radiation
,
Lrad
1 2
4πρ
2.2.
Boundary
conditiononapproximation,
where
the
temperature
gradient
canbedescribed
asε̄=+(vequatr +v
n respectively.
total, we have
4 constraint
equationsequations(Eqs. 14) and
3andordinary
diﬀerential
In
total,
wehave
4
constraint
(Eqs.
14)
3
ordinary
diﬀerential
equat
2
Ṁ
being theAradial
Alfvénvelocity,
rotating
magnetic
wind
condition at the
bles
(ρ,
v
,
v
,
B
,
B
,
T,
L
).φ , T, Lrad9) for 7rvariables). solution has to satisfy the regularityφr (ρ,φvr , vφ , B
rad
r, B
B
φ
κρLradIn total,
Lamers & CassinellidT1999). respectively.
The AlfvénradiusrA A
isφwhereweequatio√ the 4AlfvénMach= have, constraint number
=
−
,
4πρ
3 r 2condition
Eqs (1), (3) and (10),be written
9) 2.2.
for 7canvariables(ρ, asvr , vφ , B
Boundaryr , Bφ , T, Lrad ).
drthe velocity
16πacλT
2.2.
Boundary
condition
being the azimuthal Alfvénvelocity, and2
A rotating magnetic wind solution has to satisfy the regularity condition at theFslow,
Alfvén, aB
2.2. amagneticwindsolutionhastosatisfytheregularity
condition
at
the
slow,
vA =flux
Ar (r =
rA ) =. Alfvén,acity, Lrad is the radiation luminosity, and λ is thelimiter.
We
calculaLrad 1ε̄ =+ (2
7 variables Ṁ

total, we have 4 constraint ees (ρ, vr , vφ , Br , Bφ , T, Lrad ).

agnetic wind solution has toA Awhich
A
r=r
r=r
A
rad
Adwarfs
B withAA
ween
massand
andequatorial
equatorial
radiusoxygen-neon
whitedwarfswith∗diﬀerent
diﬀerent
angularIn
ial mass
direction,
for
the
mass
loss
rate
and
radialvelocityarethe largest.
enradiusofof
oxygen-neon
white
angularumericalsolutionspassingr = rA aregiven
not byphysicalwind solution;a windatorialRadius[cm]
the fixing
terminal
isr=rapproximatelytheso-called
Michelvelocity;
with(rAvelocity, du/dx|
,
Ṁ
,
T
(r
),
L
(r
),
F
,
Ω,
M
),
we
can
obtain
A
rad A
B
∗
A
8 in Eq. (8)and fast
points where
coeﬃcient
dvr /drzero, i.e.,
8 8solutions
8 8 ther5x10
8r8 areof6x10
8physical
8 8becomes
ericalpassing=notwindsolution;
#
$
3x10
4x10
7x10
A
−1/3a wind
3x10
4x10
5x10
6x10
! a solution"!to be regular"4/3!these"2/3 the7x10
2/3
0.al
For
at
points,
right
hand
side
of Eq.InIn(8)
rial
direction,
for
which
the
mass
loss
rate
and
radialvelocityarethelargest.
direction,
for
which
the
mass
loss
rate
and
radialvelocityarethelargest.
B
R
Ω
Ṁ
∗
∗
ds−1
fast points where the coeﬃcient of dvr /dr in Eq. (8) becomes zero,i.e.,.
itionalconstraints
on
the
wind
solution.
Herewechanger
anddu/dx|
uatorial
Radius[cm]
A
r=r, theterminal
terminal
velocity
isapproximately
approximately
givenbybythetheso-called
Michelvelocity;(22)8 G velocity−1−6 M Michel−1 velocity;A
atorialRadius
[cm]
the
is
given
so-called
10
1,
500
km
1
s
3
×
10
yr
⊙ side of Eq. (8)For a solution to be regular at these points, the right handparameter set of (Ṁ , T (rA ), Lrad (rA ), FB , Ω,
M∗ ).
#
#
$$
−1/3
onal
constraints
on
the
wind
solution.
Herewechanger
anddu/dx|
!
"
!
"
!
"
−1/3
A
r=rA
!
"
!
"
!
"
2/3
4/3
2/3
2/3
4/3
2/3
we
have
5
additional
constraints.
First,
the
mass
loss
rate
has
to
be
consistent
BRΩṀ
constraint
on
F
Ω.
Third
and
fourth,theradiation
temperatureandluminosity
∗
∗
B
R
Ω
Ṁ
B
∗ ), L
−1
of
(
Ṁ
,
T
(r
(rA ), −1Fmrameters−1 •∗set(22)
Go
throughpoint
A theradslow
B , Ω, M∗ ).
. . (22)
8G−6 M yr
−1
8
−1
−6
−1
10
1,
500
km
1
s
3
×
10
values.
In order 1,
toconstraints.
be consistentthenon-detectionof
PbeCygni
profile,
⊙
10
G
500
km
1also
s with3×
10 rateM⊙ hasyr
have
5 additional
First,
the
mass
loss
to
consistent! Ṁobs. the(20)
mparableor Ṁslightlylargerthan
thepoint
Alfvénradius. This leads to• Go
throughfast
l constraintononFF
Thirdandandfourth,fourth,thetheradiation
radiationtemperaturetemperatureandandluminosity
luminosity
constraintΩ.Ω.ThirdBBdhas to beṀconsistentwiththeobserved
value;! Ṁto(20)•InInorderdvalues.
values.
order
consistentalsowith
withthethenon-detection
non-detectionofofPPCygni
Cygniprofile,profile,T (r∼be.consistentTeﬀ,obs, also(23)to)obsbephomparableslightlylargerthan
theAlfvénradius.
Alfvénradius.
Thisleads
leadstoto
mparablethevorrslightly(∞)! largervwith. than(21)
as to beconsistentobserved
value; This∞,obsthe• or
Lrad (rph ) ∼ Lrad,obs .
(24)) ∼Teﬀ,obs
Teﬀ,obs
(23)
ph
TT
(r(r
) v∼
, ,
(23)
ph
•
v
(∞)
!
.
(21)
r
∞,obs
ition; at the surface of the degenerate core, the wind is powered by the nuclear

7 boundary conditions

e shouldequal
theradiation
luminosity;
Lrad
) ∼L
Lrad,obs
(r(r
) to
∼
. .
• Lberadphph
rad,obs(24)(24)

dition;thesurface ofrad
thedegeneratecore,thethewindwindisispowered
poweredbybythe
thenuclear
nucleartion; at•atthe
degenerate
core,
Lsurface(R(25)
n (R∗ ) ≈ofLthe∗ ).
teshould
shouldbebeequal
equaltotothe
theradiation
radiationluminosity;
luminosity;
• The
M*-R
relationrotatingcore et al. (2012).
ytic fitting
formulafor*thecarbon ofburninggiven ONein Kippenhahn
) ≈L
Lrad
(25)
n (R
(R
(R(R
).∗ ).
∗ )∗ ≈
rad∗parameters0-25), theLnL
residualmodel
are the mass M∗ and (equatorial)(25)
radiuse specify the M∗ -R∗ relation, a sequence of wind solutions for WD J005311
lytic
fittingformula
formulafor
forthethecarbon
carbonburningburninggiven
givenininKippenhahn
Kippenhahnetetal.al.(2012).
(2012).
tic fittingThe M*-R* relation of uniformly rotating ONe core
1.45
1.4

Mass [Solar mass]

1.35
1.3
No RotationΩ = 0.1 [s-1]-1Ω = 0.5 [s ]
Ω = 0.75 [s-1]Ω = 1.0 [s-1]-1Ω = 1.5 [s ]
Ω = 2.0 [s-1]Ω = 3.0 [s-1]Ω = 6.0 [s-1]
Near Criticalρc = 1x109 [g cm-3]

1.25
1.2
1.15
1.1
1.05
1
0

8

1x10

8

2x10

8

8

8

3x10
4x10
5x10
Equatorial Radius [cm]

8

6x10

8

7x10

Fujisawa 15

Results

Azimu2x108

The WD J005311 wind : vr & vφ

1x108

Wind from WD J005311
6x108

1x109

1x10101x1011Radius r [cm]9

1.5x10

9

1x10

1x109

vr

5x108

8

1x10

0
8
1x10

1x10

9

10

11

1x10
1x10
Radius r [cm]1x1012
5x108
Azimuthal velocity vφ [cm s-1]

Radial velocity vr [cm s-1]

2x109

3x108
8

vr

2x10

0
8
1x10

12

1x10

10

9

1x10

10

1x10
1x10
Radius r [cm]

11

12

1x10

9

1x10

1x10

1x108
6

1x10

10000

1x106

100

vφ

1

100000 0.01
81x101x10
8

9
1x10
9

Azimuthal velocity vφ [cm s-1]

1x10

4x108

1x108

7

Radial velocity vr [cm s-1]

Log scaleAzimuthal velocity vφ [cm s-1]

Liner scale

2.5x109

0
1x108

7

1x108

1x107

1x106

11
1000001x1010 11
1x10
1x1012
12
8
9
10
11
1x10
1x10 right
1x10 panels
1x10
1x10
netic wind solution compatible with WD J005311. The left andRadius r [cm]Radius r [cm]
1x10

10

1x10
1x10
Radius r [cm]

vφ
1x10

12

ely. The top and bottom panels are in liner and log scale, respectively. We
876
Figureof therotating
solution
with
WD
The =
left 6andth M∗ = 1.25
M⊙3., TheR∗ velocity= 3.3profile× 10
cm,
B∗magnetic= 4.2wind
× 10
G,compatibleΩ = 0.5s−1, J005311.
and Ṁ
⇥right10 panels
M yr 1
are the radial and azimuthal components, respectively. The top and bottom panels are in liner and log scale, respectively. We<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>

8

7

1

Azimu2x108

The WD J005311 wind : vr & vφ

1x108

Wind from WD J005311
6x108

1x109

1x10101x1011Radius r [cm]9

1.5x10

9

1x10

1x109

vr

5x108

8

1x10

0
8
1x10

1x10

9

10

11

1x10
1x10
Radius r [cm]1x1012
5x108
Azimuthal velocity vφ [cm s-1]

Radial velocity vr [cm s-1]

2x109

3x108
8

vr

2x10

0
8
1x10

12

1x10

10

9

1x10

10

1x10
1x10
Radius r [cm]

11

12

1x10

9

1x10

1x10

1x108
6

1x10

10000

1x106

100

vφ

1

100000 0.01
81x101x10
8

9
1x10
9

Azimuthal velocity vφ [cm s-1]

1x10

4x108

1x108

7

Radial velocity vr [cm s-1]

Log scaleAzimuthal velocity vφ [cm s-1]

Liner scale

2.5x109

0
1x108

7

1x108

1x107

1x106

11
1000001x1010 11
1x10
1x1012
12
8
9
10
11
1x10
1x10 right
1x10 panels
1x10
1x10
netic wind solution compatible with WD J005311. The left andRadius r [cm]Radius r [cm]
1x10

10

1x10
1x10
Radius r [cm]

vφ
1x10

12

ely. The top and bottom panels are in liner and log scale, respectively. We
876
Figureof therotating
solution
with
WD
The =
left 6andth M∗ = 1.25
M⊙3., TheR∗ velocity= 3.3profile× 10
cm,
B∗magnetic= 4.2wind
× 10
G,compatibleΩ = 0.5s−1, J005311.
and Ṁ
⇥right10 panels
M yr 1
are the radial and azimuthal components, respectively. The top and bottom panels are in liner and log scale, respectively. We<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">AAAClXichVHLShxBFD12otHR6BgXCtk0DkoWOtwOYoIgSBIkG/GV0YFpHbrbmrGwX3TXDEya+YF8QLLISkEk5BeykwR/wIWfELI0kE0W3ulpECPR23TVqXPvuXWqyg5dGSuiix7twcPevkf9A7nBocfDI/nRJ1tx0IgcUXICN4jKthULV/qipKRyRTmMhOXZrti2D1538ttNEcUy8N+pVih2PKvuy5p0LMVUNU/mXqD0FX1RnzeV9ESsG7SbzM63zZmVqhlw0pxJzMjTWxHTRrtdzReoSGnot4GRgQKyWAvyJzCxhwAOGvAg4EMxdmEh5q8CA4SQuR0kzEWMZJoXaCPH2gZXCa6wmD3gsc6rSsb6vO70jFO1w7u4/Ees1DFF5/SFLumMvtJP+vvfXknao+OlxbPd1YqwOvJhYvPPvSqPZ4X9a9WdnhVqeJl6lew9TJnOKZyuvvn+0+XmwsZUMk1H9Iv9H9IFnfIJ/OZv53hdbHxGjh/A+Pe6b4Ot50WDisb6XGHpVfYU/XiKSTzj+36BJbzFGkq870d8w3f80Ma1Re2Nttwt1XoyzRhuhLZ6BTNqmsM=</latexit>

8

7

1

Azimu2x108

The WD J005311 wind : vr & vφ

1x108

Wind from WD J005311
6x108

1x109

1x10101x1011Radius r [cm]9

1.5x10

9

1x10

1x109

vr

5x108

8

1x10

0
8
1x10

1x10

9

10

11

1x10
1x10
Radius r [cm]1x1012
5x108
Azimuthal velocity vφ [cm s-1]

Radial velocity vr [cm s-1]

2x109

3x108
8

vr

2x10

0
8
1x10

12

1x10

10

9

1x10

10

1x10
1x10
Radius r [cm]

11

12

1x10

9

1x10

1x10

1x108
6

1x10

10000

1x106

100

vφ

1

100000 0.01
81x101x10
8

9
1x10
9

Azimuthal velocity vφ [cm s-1]

1x10

4x108

1x108

7

Radial velocity vr [cm s-1]

Log scaleAzimuthal velocity vφ [cm s-1]

Liner scale

2.5x109

0
1x108

7

1x108

1x107

1x106

11
1000001x1010 11
1x10
1x1012
12
8
9
10
11
1x10
1x10 right
1x10 panels
1x10
1x10
netic wind solution compatible with WD J005311. The left andRadius r [cm]Radius r [cm]
1x10

10

1x10
1x10
Radius r [cm]

vφ
1x10

12

ely. The top and bottom panels are in liner and log scale, respectively. We
876
Figureof therotating
solution
with
WD
The =
left 6andth M∗ = 1.25
M⊙3., TheR∗ velocity= 3.3profile× 10
cm,
B∗magnetic= 4.2wind
× 10
G,compatibleΩ = 0.5s−1, J005311.
and Ṁ
⇥right10 panels
M yr 1
are the radial and azimuthal components, respectively. The top and bottom panels are in liner and log scale, respectively. We<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>

8

7

1

Azimu2x108

The WD J005311 wind : vr & vφ

1x108

Wind from WD J005311
6x108

1x109

1x10101x1011Radius r [cm]9

1.5x10

9

1x10

1x109

vr

5x108

8

1x10

0
8
1x10

1x10

9

10

11

1x10
1x10
Radius r [cm]1x1012
5x108
Azimuthal velocity vφ [cm s-1]

Radial velocity vr [cm s-1]

2x109

3x108
8

vr

2x10

0
8
1x10

12

1x10

10

9

1x10

10

1x10
1x10
Radius r [cm]

11

12

1x10

9

1x10

1x10

1x108
6

1x10

10000

1x106

100

vφ

1

100000 0.01
81x101x10
8

9
1x10
9

Azimuthal velocity vφ [cm s-1]

1x10

4x108

1x108

7

Radial velocity vr [cm s-1]

Log scaleAzimuthal velocity vφ [cm s-1]

Liner scale

2.5x109

0
1x108

7

1x108

1x107

1x106

11
1000001x1010 11
1x10
1x1012
12
8
9
10
11
1x10
1x10 right
1x10 panels
1x10
1x10
netic wind solution compatible with WD J005311. The left andRadius r [cm]Radius r [cm]
1x10

10

1x10
1x10
Radius r [cm]

vφ
1x10

12

ely. The top and bottom panels are in liner and log scale, respectively. We
876
Figureof therotating
solution
with
WD
The =
left 6andth M∗ = 1.25
M⊙3., TheR∗ velocity= 3.3profile× 10
cm,
B∗magnetic= 4.2wind
× 10
G,compatibleΩ = 0.5s−1, J005311.
and Ṁ
⇥right10 panels
M yr 1
are the radial and azimuthal components, respectively. The top and bottom panels are in liner and log scale, respectively. We<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>

8

7

1

Azimu2x108

The WD J005311 wind : Br & Bφ

1x108

0
1x108

Magnetic field strength [G]Azimuthal velocity vφ [cm s-1]

1x109

8 9

1x10
1x10

1x1012

1x106

1x108

10000

7

100

1x10

1x10101x1011Radius r [cm]

Br
-Bφ

1
6

1x10

100000
1x108

0.01
1x108
1x109

1x109

1x10101x1011r [cm]
1x1011 Radius
1x1012

1x1012

1x1010netic wind solution compatible with WD J005311. The left and right panels
Radius r [cm]ely. The top and bottom panels are in liner and log scale, respectively. We
th M∗ = 1.25 M⊙ , R∗ = 3.3 × 108 cm, B∗ = 4.2 × 107 G, Ω = 0.5 s−1 , and Ṁ = 6 ⇥ 10 6 M yr 1
<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>Temperature T [K

Azimu

2x108

The WD J005311 wind : ρ, T, Lrad8

1x10

Kashiyama et al.

100000

0
1x108

ρ

1x109

1x10101x1011Radius r [cm]Density ρ [g cm-3]

1

1x107

1x106

1x1012
100000
1x108

1x109
1x10

-5

1x109

1x10101x1011Radius r [cm]2.1x1038

Lrad

1x10-10

1x10

9

10

11

1x10
1x10
Radius r [cm]

1x109

12

1x10

T

7

1x10

8

1x10

Luminosity Lrad [erg s-1]

8

1x10

Temperature T [K]Azimuthal velocity vφ [cm s-1]

38

8
1x10
1x10-15

2.05x102x10381.95x1038

1.9x1038
1x108

1x10671x10

1x1012

1x109

1x10101x1011Radius r [cm]1x10126

1x10

Figure 4. The density, temperature, and radiation luminosity of the wind solution

1000008100000
1x10
8
1x10

10
1x10
1x10111x1012
11
12
1x10
1x10
netic wind solution compatible
with WD J005311. The left and right panels
Radius r [cm] Radius r [cm]
1x10

9

9
1x101x10
10ely. The top 2.1x10
and bottom panels are in liner and log scale, respectively. We
th M∗ = 1.25 M⊙ , R∗ = 3.3 × 108 cm, B∗ = 4.2 × 107 G, Ω = 0.5 s−1 , and Ṁ = 6 ⇥ 10 6 M yr 1
38

<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>Temperature T [K

Azimu

2x108

The WD J005311 wind : ρ, T, Lrad8

1x10

Kashiyama et al.

100000

0
1x108

ρ

1x109

1x10101x1011Radius r [cm]Density ρ [g cm-3]

1

1x107

1x106

1x1012
100000
1x108

1x109
1x10

-5

1x109

1x10101x1011Radius r [cm]2.1x1038

Lrad

1x10-10

1x10

9

10

11

1x10
1x10
Radius r [cm]

1x109

12

1x10

T

7

1x10

8

1x10

Luminosity Lrad [erg s-1]

8

1x10

Temperature T [K]Azimuthal velocity vφ [cm s-1]

38

8
1x10
1x10-15

2.05x102x10381.95x1038

1.9x1038
1x108

1x10671x10

1x1012

1x109

1x10101x1011Radius r [cm]1x10126

1x10

Figure 4. The density, temperature, and radiation luminosity of the wind solution

1000008100000
1x10
8
1x10

10
1x10
1x10111x1012
11
12
1x10
1x10
netic wind solution compatible
with WD J005311. The left and right panels
Radius r [cm] Radius r [cm]
1x10

9

9
1x101x10
10ely. The top 2.1x10
and bottom panels are in liner and log scale, respectively. We
th M∗ = 1.25 M⊙ , R∗ = 3.3 × 108 cm, B∗ = 4.2 × 107 G, Ω = 0.5 s−1 , and Ṁ = 6 ⇥ 10 6 M yr 1
38

<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>Temperature T [K

Azimu

2x108

The WD J005311 wind : ρ, T, Lrad8

1x10

Kashiyama et al.

100000

0
1x108

ρ

1x109

1x10101x1011Radius r [cm]Density ρ [g cm-3]

1

1x107

1x106

1x1012
100000
1x108

1x109
1x10

-5

1x109

1x10101x1011Radius r [cm]2.1x1038

Lrad

1x10-10

1x10

9

10

11

1x10
1x10
Radius r [cm]

1x109

12

1x10

T

7

1x10

8

1x10

Luminosity Lrad [erg s-1]

8

1x10

Temperature T [K]Azimuthal velocity vφ [cm s-1]

38

8
1x10
1x10-15

2.05x102x10381.95x1038

1.9x1038
1x108

1x10671x10

1x1012

1x109

1x10101x1011Radius r [cm]1x10126

1x10

Figure 4. The density, temperature, and radiation luminosity of the wind solution

1000008100000
1x10
8
1x10

10
1x10
1x10111x1012
11
12
1x10
1x10
netic wind solution compatible
with WD J005311. The left and right panels
Radius r [cm] Radius r [cm]
1x10

9

9
1x101x10
10ely. The top 2.1x10
and bottom panels are in liner and log scale, respectively. We
th M∗ = 1.25 M⊙ , R∗ = 3.3 × 108 cm, B∗ = 4.2 × 107 G, Ω = 0.5 s−1 , and Ṁ = 6 ⇥ 10 6 M yr 1
38

<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>Temperature T [K

Azimu

2x108

The WD J005311 wind : ρ, T, Lrad8

1x10

Kashiyama et al.

100000

0
1x108

ρ

1x109

1x10101x1011Radius r [cm]Density ρ [g cm-3]

1

1x107

1x106

1x1012
100000
1x108

1x109
1x10

-5

1x109

1x10101x1011Radius r [cm]2.1x1038

Lrad

1x10-10

1x10

9

10

11

1x10
1x10
Radius r [cm]

1x109

12

1x10

T

7

1x10

8

1x10

Luminosity Lrad [erg s-1]

8

1x10

Temperature T [K]Azimuthal velocity vφ [cm s-1]

38

8
1x10
1x10-15

2.05x102x10381.95x1038

1.9x1038
1x108

1x10671x10

1x1012

1x109

1x10101x1011Radius r [cm]1x10126

1x10

Figure 4. The density, temperature, and radiation luminosity of the wind solution

1000008100000
1x10
8
1x10

10
1x10
1x10111x1012
11
12
1x10
1x10
netic wind solution compatible
with WD J005311. The left and right panels
Radius r [cm] Radius r [cm]
1x10

9

9
1x101x10
10ely. The top 2.1x10
and bottom panels are in liner and log scale, respectively. We
th M∗ = 1.25 M⊙ , R∗ = 3.3 × 108 cm, B∗ = 4.2 × 107 G, Ω = 0.5 s−1 , and Ṁ = 6 ⇥ 10 6 M yr 1
38

<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>

Azimu

2x108
1x108
0
1x108

8

The WD J005311 wind :How is it accelerated?
1x109

1x10101x1011Radius r [cm]1x1012

Kashiyama et al.

9

1x10

1x10201x1019

1x108

1x108

vr
vφ
Ar
-Aφ
rΩ
cs
vesc

7

1x10

Energy density [erg/g]

Azimuthal velocity vφ [cm s-1]

Velocity [cm s-1]

1x109

1x10181x1017εεB
εK

1x1016

εrad
εgas
-εG

1x10151x1014

1x107

1x106

1x10

8

1x10

9

10

1x10

1x10

11

Radius r [cm]

1x10

12

1x1013
1x108

1x109

1x10101x10111x1012Radius r [cm]Figure 4. 100000
Left: Comparisonof theradial and8910 azimuthal11velocities of
12the wind solution in Fig. 3 with other relevant velocities
1x10
1x10
1x10
1x10
1x10
includingradial (Acompatible) Alfvénvelocities,
velocityr ) and azimuthal
neticwindthesolution
with(AWD
J005311.
Thetheleftcorotation
and right
panelswith the degenerate core (r⌦), theRadiusr[cm]
adiabatic sound velocity of the gas (cs ), and the escape velocity (vesc ). Right: The radial profile of the energy density of theely.
The top and bottom panels are in linerfrom
andmagneticlog scale,respectively.
We (" ), radiation (" ), thermal gas
wind solution in Fig. 3. We show the contributions
field
("
),
kinetic
energy
B
K
rad
8
7
−1
6
th
M),∗ and= 1.25M⊙ , Renergy
M yr 1∗ = 3.3("gas
gravitational("G×). 10 cm, B∗ = 4.2 × 10 G, Ω = 0.5 s , and Ṁ = 6 ⇥ 10<latexit sha1_base64="ekZg6D+feY4gI9Bfg65UgdYeP5E=">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</latexit>

The WD J005311 wind :Allowed parameter region
Wind from WD J005311
1.4

White Dwarf Mass M* [M ]Surface magnetic field B* [G]

1x108

.
-6
-1
vr(∞) = 2.4x109 cm s-1, M. = 6x10 M yr
9

-1

-6

1.35
1.3
1.25
1.2
1.15
1.1
1.05

-6
-1
vr(∞) = 1.9x109 cm s-1, M. = 6x10 M yr
-1vr(∞) = 2.4x10 cm s , M = 3x10 M yr

1
2x108

7

1x10

9

0.1

3x108

4x108

5x108

1
-1

Equatorial Radius of White Dwarf R* [cm]Spin angular frequency Ω [s ]Figure 5. White dwarf parameters that give wind solutions compatible with WD J005311. The left and right panels show
surface magnetic field and spin angular frequency (B⇤ , ⌦) and mass and radius (M⇤ , R⇤ ), respectively.

The observed properties of WD J005311 can be explained by
the rotating magnetic wind from an ONe WD with
M . 1.3 M as long as assuming that v (1) is non-relativistic. The low mass end are also set by Eq. (27); a smaller−1. r > r
the WD masslarger r M
becomes,the condition r7 G,< r andbreaks.
Even if accepting
Mbecomes,= (2-5)×10
Ω = 0.2-0.5s∗ = 1.1-1.3⊙, B∗ and
⇤

r

A

A

ph,obsAph,obsand taking smaller M⇤ , we find that the carbon burning no longer ignites on the surface for M⇤ . 1.1 M . ThisKashiyama, Fujisawa, Shigeyama 19
Wind from WD J005311

Slow point

Alfvén point

3

Photosphere

Fast point

C burning

vr ⇠ 108 cm s 1

vr . v1 = a few ⇥ 109 cm s 1

vr ⇡ v1

ONecoreM⇤ = 1.1-1.3 M⌦ = 0.2-0.5 s 1

B⇤ = (2-5) ⇥ 107 G

rs ⇠ 109 cm

rA . rph ⇠ 1010 cm

Figure 1. Schematic picture of our wind model for white dwarf J005311.

rs & 1012 cm

arXiv:1907.12317

Lessen learned• WD J005311 will neither explode as type Ia
supernova nor collapse into neutron star.
• If the wind continues to blow another a few kyr,WD J005311 will spin down significantly and join to
the known sequence of slowly-rotating magnetic
WDs.
• Otherwise it may appear as a fast-spinning magnetic
WD and could be a new high energy source.
• The photosphere spins with a period of ~min.

Still, there should be ~ 100 of
massive WD merger remnantsin the Galaxy…

(the Hertz Spinning Object survey)

withSearching for yet-to-be-discovered
sub-minute variability of white dwarfs• Spin (close to the mass shedding limit)ü (Magnetohydro)dynamics of formation and mergerü A new class of high energy source• (p-mode) oscillation
ü New asteroseismology to probe the interior• Tidal disruption (of asteroids)• Transits (of “habitable” planets)
üFuture of our solar system?

Tomo-e observation of J005311

Timing analysis of J005311

The survey has started (~50TB/night).
The pipeline construction underway …

We need more people. If you are interested in the data, please let me know!