Fe1 pc(c) T~15 Myr

Collapse (∆ C ~ 105 yr)

CAI (~ 104 yr)

26Al injec!onIn the following, we show that such a scenario presents many realizations that permit a good fit of the quantities of 26 Al and 60 Fe
at the solar system’s birth. In that respect, it provides a morenatural explanation than previous models, because it does not
require special and/or unlikely conditions, and leads to understanding how the solar system forms within a broader perspective. The key point is that 60 Fe comes from the SNe of the first
generation of stars, while 26 Al comes from the wind of a single massive star belonging to a second star generation. Thisdecoupling between the sources of 60 Fe and of 26 Al is essential
to explain the observed 26 Al/60 Fe ratio when the solar system– At t ∼ 10 Myr, a second star generation (#2, containing a
total of N2 stars) forms in region #2, partly due to the compressive action of the generation #1 SNe shockwaves onto
the molecular cloud gas (Preibisch & Zinnecker 2007) (seepanel b of Fig. 1).
– From t ∼ 10 Myr and for some Myr, the wind of one or
two massive stars from generation #2 will collect ISM gas
to build a dense shell surrounding an HII region of radius
5−10 pc (Deharveng et al. 2010). That collected shell, whichcontains 60 Fe originating in the SNe of the first generation,
will be wind-enriched in 26 Al via efficient turbulent mixing (Koyama & Inutsuka 2002) during a time t! lasting afew Myr (see Fig. 2).
– At t ∼ 10 Myr + t! , aluminum-26 delivery ends when
the dense shell fragments and collapses via a diversity ofgravito-turbulent mechanisms, such as gravitational instabilities and ionization of a turbulent medium (Deharveng et al.
2010), to form a third generation star cluster (#3). The collapse phase lasts ∆C ∼ 105 yr. Our Sun belongs to that thirdgeneration of stars (see panel c of Fig. 1). CAIs formed in theprotoplanetary disk surrounding the protoSun on a timescaleof a few 104 yr (Jacobsen et al. 2008) contains 26 Al fromthe wind of the generation #2 massive star and 60 Fe from thegeneration #1 SNe (Fig. 2).

Fig. 2. Timeline for Al injection in a dense collected shell around a
massive star, starting approximately 10 Myr after the birth of stellar
generation #1 and lasting ∼t! . The upper part of the figure represents
the time line of the central massive star of panel c in Fig. 1. In the middle part, the timeline of the 26 Al production and injection (arrows) isshown. Aluminum-26 is present in the wind some 105 yr after the starformation and absent when products of helium-burning appear at thesurface (WC-type star) since 26 Al is destroyed in helium-burning cores.
It is present while the star explodes as an SN. Aluminum-26 injectionin the shell lasts during the whole collection phase and is assumed tostop during the collapse phase lasting a time ∆C ∼ 105 yr. The lower
part represents the timeline of the collected shell, which eventually collapses to produce a protoSun and a protoplanetary disk in which mostCAIs form.

26

Collect (t! ~ few 106 yr)

26Al produc

ー半減期が100Myrより短い short-lived radionuclides, SLRsを使って、太陽系の歴史を考える
ーSLRsは、その起源は知られていて、4.56Gyr前に太陽系原始円盤で存在し、歴史を調べる指標となる
ー以前のモデルでは、26Al(1.1Myr)と60Fe(3.7Myr)の存在比を妥当的な説明ができていなかった
ー最近の星形成の理解に基づき、これらの元素について、妥当的な解釈を与えるのが目的
ーー60Fe、太陽系初期に、GMC(巨大分子雲)で第一世代に属する超新星爆発の多様性によって供給されたことが知られている
ーー26Al、第二世代の単一の大質量星星風により高密度シェルに供給される
ーー太陽は、第三世代としてシェルで形成されたーこの論文で26Alは(ウォルフライエだけでなく)主系列星の星風に存在する新しい星のモデルにより供給されるーこの論文のシナリオでは、太陽系形成に先行する二つの世代の(星の数とともに)時系列を制限する
ーそのモデルで、太陽系原始円盤でのさまざまな半減期を持つ存在は階層的星間物質内(ISM)の主系列星形成の化石化記録[隕石]の他にない。
ー太陽は、 1200個程度のクラスターに属す 30太陽質量以上の元の大質量星から5-10pcの距離にある高密度シェルで数100個の星とともに生またことを示す。

Fig. 1. Sketch of the model described in Sect. 2. Star generations #1,#2, and #3 are respectively in red, blue, and green. In panel b), SNeremnants are shown with a dark contour. The reddish background symbolizes 60 Fe delivered by the SNe belonging to the first star generation.
In panel c), the purple color of the shell symbolizes the combinationof 26 Al delivered by the single massive star wind from generation #2
and the 60 Fe delivered by generation #1 stars. Our Sun, born in the circumstellar shell together with a few hundreds fellow low-mass stars(generation #3), is shown in yellow.

10 pc(b) T~10 Myr

Fe6060SN	10 pconWR	(a) T=0Main sequence (O)M. Gounelle and G. Meynet: Solar system genealogy revealed by extinct short-lived radionuclides in meteorites

・Collisional Excitation of the [CII] Fine Structure Transition in Interstellar Clouds
Paul F. Goldsmith, William D. Langer, Jorge D. Pineda and Thangasamy Velusamy

ーCII (C+) 158μm(1900.5GHz)微細構造線の衝突励起の計算
ーCII (C+)輝線は、ーーPDRやISMで重要なcoolantーー銀河系や系外銀河で星形成のトレーサー
ーー分光観測、HershcelのHIFI、SOFIAのGREATーーー解析で、同位体C13+の放射と混ざったり相対的に弱いため、光学的厚みを決定することが難しい
ーで、CII 輝線の輻射輸送と励起のLVGの解析的結果と数値計算ーー単純な分子雲(一様の密度、運動温度、衝突係数)を仮定
ーーガスの運動温度の1/3の輝度温度までのアンテナ温度で、光学的厚みに関わらず、C+の柱密度に比例する＝＞eﬀectively optically thin (EOT) approximation
ーーさまざまな衝突パラメータでC+輝線の励起臨海密度について考え、簡単にC＋吸収を解析し、強度の考慮がISMの冷却の振る舞いにどのように影響するか議論する

・Solar system genealogy revealed by extinct short-lived radionuclides in meteorites
Matthieu Gounelle and Georges Meynet

stars.

a few
hundredstars
in a dense
collectedofshellnsecollectedshellsituated
at a distance
5-10situated
pc of a at a distance of 5-10 pc of asslarger
thanabout30
solarmasses,andbelonging
to a incluster
containing∼ 1200r masses, and belonging to a cluster
containing∼ 1200Acceptedby Published
Astronomy& Astrophysics
545 A4 (2012)

http://www.aanda.org/index.php?option=com article&access=doi&doi=10.1051/0004-6361/201219031
nomy& Astrophysics 545 A4 (2012)(2012)

article&access=doi&doi=10.1051/0004-6361/201219031&Itemid=129
p?option=com=doi&doi=10.1051/0004-6361/201219031&Itemid=129
・Discoveryof an outflow of the very low-mass star ISO 143

Discovery of an outflow of the very low-mass star ISO 143

V. Joergens, T.V.
Kopytova
and1,2A., PohlJoergens
T. Kopytova2 and A. Pohl2	starISO
143low-mass star ISO 143ofthevery
1

Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-UeberlstarのISO143でアウトフローを発見
and A. Pohl2ーvery low-massHeidelberg,
GermanyーーUVES/VLT、禁制線[SII](6716Å,6731Å)2
Astrophysik,Albert-Ueberle-Str.
2,Institut
69120 Albert-Ueberle-Str.
mTheoretischefür Astronomie,Institut für
TheoretischeAstrophysik,
2, 69120 17, 69117 Heidelberg, Germany
Max-Planckfür Astronomie, Königstuhl
ーーー200-300mas(30-50AU) の空間構造、50-70km/sの速度レンジを観測
E-mail contact: viki at mpia.deHeidelberg,
Germany
nomie,
Königstuhl
17, 69117 Heidelberg,
Germanyーーー他、Ca
II(8498Å),OI(8446Å),He I(7065Å),弱い[Fe II](7155Å)を検出
We discover that the very young very low-mass star ISO 143 (M5) is driving an outflow based on spectroーISO143
forbidden [S II] emission lines at 6716 Å and 6731 Å observed in UVES/VLT spectra. ISO 143 is only onM5) is driving anーーアウトフローが検出され、Toutflow based on spectro-astrometryof phaseにある、
taurivery low-mass star ISO 143 (M5) isofdriving
andwarfs
outflow
based
spectro-astrometryof for which an outflow has been detected and that
brown
and
veryonlow-massstars (M5-M8)
n UVES/VLT spectra. ISO 143 is only
one ofa handful
6716 Å and 6731 Å observed
inUVES/VLT
spectra.
ISO143is
only
oneofahandful
T thatTauriphasethat
continues
at verylow masses. We have found the outflow of ISO 143 to be intrinsically as数少ないbrowndwarf、very
low-massstar(M5-M8)
an outflow has been
detected andshow
theassstars(M5-M8)
for
which
anoutflowhas
been
detectedandthatthat asthetheaccretion
disk
tonot
obscuretheshow
outflow,solely the red outflow component is visible in the [S II]
ーー非対称なアウトフローと降着円盤を発見
he outflow of ISO
143 to be intrinsically asymmetric andowmasses.
We
have
found
theoutflowofISO143
tobeintrinsicallyasymmetricand
is [SonlythethirdT143
Tauri object showing a stronger red outflow component in spectro-astrometry, after
outflow component
isvisible
intheII]lines.
ISOーー([Soutflow, astheII]で)アウトフローはred成分のみ見える
red outflow
componentis(G5)
visibleWein the[S II]
lines.
143andISORW
217Aur(M6.25).
show
here
thatISO
including
ISO 143 two out of seven outflows confirmed inwthe
component
insolely
spectro-astrometry,
after
ーー分光観測で強いredアウトフロー成分を持つTtauriでRW
Aur(G5)とISO217(M6.25)に続く３天体
showingstrongeroutflow
componentin spectro-astrometry,after RWasymmetric.
Aur (G5) We measure a spatial extension of the outflow inmassinregime(M5-M8)two outa ofseven red
outflows
confirmed
thevery
low- are intrinsically
V. Joergens, T. Kopytova, A. Pohl: Discovery of an outflow of the very low-mass star ISO 143
herea that
includingout ofoutflows
confirmed
in velocities
the very lowーlineISO
proﬁle解析を行い、
surespatialextensionof143
thetwooutflow
in seven[SII] (aboutofup to30-50
200-300masAU) andof up to 50-70 km s−1 . We detect furthermore line emiss
Table 2. Observed emission lines of ISO 143.
sicallyWe II；
measureainspatial
extensionofI theoutflow
inI [SII] ofÅ),
upandto weaklyinfall
m s−1 . asymmetric.
We detectfurthermore
lineemissionof ISO
Ca II(8498Å), 143
O(8446Å), He(7065in [Fezone)に寄与する
II] (7155 Å). We demonstrate based oーーCa
変動する風、彩層活動、磁気圏落下ゾーン(magnetosphericline
blue component
green component
red component
ndof up
50-70 km s−1based. We ondetectfurthermore
lineemissionofII ISO
143slit PAcandatebe attributed[Fe velocitiesII] (7155 Å).
Wetodemonstratea lineprofile
analysis
anddecomposition
that
theCa
emissiona variaV
FWHM EW toV chromospheric
FWHM EWVFWHMactivity,EWーーO I : 降着に関係、ただし星風にも関係する[km/s][km/s][Å] [km/s][km/s][Å] [km/s][km/s][Å][deg]tributed
chromosphericactivity,avariable
wind,
andHe
I (7065toÅ),and weaklyV.in[FeII](7155Å).
We
demonstrate
based
on
aline
profilethemagnetosphericinfallzone,
theOI
emission
mainlyto
accretion-related
processes
but
also
awind
Joergens, T. Kopytova, A. Pohl: Discovery of an outflow of the very low-mass star ISO 143[S II]
3.1
2009 01 15
...
...
...
...
...
...
40.8
27.3
-0.2
ーーH
; 彩層の放射とコロナ活動
ccretion-related
processes
butalso emission
a wind,andthe He Iactivity,
the Ca II emission
can Ibeattributed
to chromosphericacoronalvariablewind,and(6716.44Å)
10.4
2008 03 19...
...
. . . outflow...
. . . rate...
41.9
28.6 of -0.2
tochromosphericoractivity.
We
estimatethemasstobe
theorderof 1
...
...
...
...
...
...
49.8
30.8
-0.2
42.2
2009 02 10−10−1ehemass
outflow rate
to betoofaccretion-related
the orderof10M
yr−82009 01 15 −9−1. . .
O I emission
mainlyprocesses
butalsoawind,
andtheHe
I
"
[SII]
3.1
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
44.2
31.7
-0.4
and the mass accretion、massrate to beof the orderof 10
to 10 . . . M. ."yr. . . .;. . thesevaluesareconsistentwit
ーmass outﬂow rate；accretion
rate；
.
...
...
44.5
26.7
-0.5
(6730.82 Å)
10.4
2008 03 19
M" activity.
yr−1 ; theseare theconsistentwith that2009 02 10
...
...
...
...
...
...
44.6
32.5
-0.4
onal
Wevalues
estimatemass
outflow
rateofandtoother
beveryof theorder ofstars.
10−10The
M"derivedyr−1 42.2 Ṁbrown
dwarfslow-mass
/
Ṁ
ratio
of
1-20
%
is
not
supporting
previout
acc
HeI
3.1
20090115.
.
.
.
.
.
.
.
.
-0.5
34.5
-0.4.
.
.
.
.
.
.
.
.
ーーこれらの値は他のbrowndwarfやlow-mass
starの値と同じ−9−1
of 1-20
supporting
previousof consistent with
...
...
...
-2.3
26.2
-0.5
...
...
...
Å)
10.4
2008 03 19eccofratio
the order
of%10is−8not
to 10
M" yr
these findings
valuesof(7065.19
otherthis ;number
to bearevery
large (>40 %)thatfor verylow-mass
42.2
2009 02objects.
10
...
...
...
2.4
28.1
-0.5
...
...
...
ts.
OI
3.1
2009 01 15
...
...
...
...
...
...
8.8
120.2
-3.7
stars. The derived
Ṁ
/
Ṁ
ratio
of
1-20
%
isnot
supporting
previous
findings
ofout
accーー
は、verylow-mass
天体でこれまで知られていた>40%の値とは違う(8446.36 Å)
10.4
2008 03 19
-42.1
61.3
-1.5
...
...
...
13.5
106.1
-2.1
...
...
...
...
...
...
18.8
121.2
-5.5
42.2
2009 02 100 %) for very low-mass objects. Accepted by A&A
Ca II
3.1
2009 01 15-1.0
60.0
-0.9
6.6
8.5
-0.1
42.0
164.8
-1.7ーーline proﬁle解析から求めた結果は、より重い星のT tauri星の特性と似ていて、browndralfである(8498.02 Å)
10.4
2008 03 19-36.3
51.1
-0.6
-1.3
20.9
-0.5
62.8
163.6-0.6
http://www.mpia.de/homes/joergens/refpublications.html
-18.4
41.4
-0.6
5.9
20.2
-0.7
25.7
94.1
-4.1
42.2
2009 02 10ISO143でTtauri phaseが継続しているだろう
Notes. The listed entries are: line with laboratory wavelength, slit PA,observing date, and for each individual component the velocity at theline peak, the FWHM, and EW. The laboratory wavelengths are taken
gens/refpublications.html
ーーアウトフローの特徴は、CTTSぽいfrom the NIST database (http://physics.nist.gov/asd3, Ralchenko et al.
KI 7699, PA=3.1 deg, 2009 01 15KI 7699, PA=10.4 deg, 2008 03 19200

KI 7699, PA=42.2 deg, 2009 02 10200

100

200

100

100-100-200-300-400-500

0counts [arbitrary units]

counts [arbitrary units]

counts [arbitrary units]

0-100
-200
-300
-400

-600

-600
0.30
0.25

-400
0.30
0.25

0.20

0.20

0.20

0.15

0.15

0.10
0.05

-0.00
-0.05
-0.10

0.15

offset [arcseconds]

offset [arcseconds]

offset [arcseconds]

-800
0.30
0.25

0.10
0.05

-0.00
-0.05
-0.10

-0.15

-0.15

-0.20

-0.20

-0.25
-0.30
-300

-0.25
-0.30
-300

-200

-100

0100
velocity [km/s]

200300

0.10
0.05

-0.00
-0.05
-0.10
-0.15
-0.20

[SII] 6716, PA=3.1 deg, 2009 01 15

-200

-100

0100velocity [km/s]

200-0.25
-0.30
-300

300

[SII] 6716, PA=10.4 deg, 2008 03 1920005002002011). The epochs are listed in the order of increasing slit PA, as in
Table 3, for clarity.

300

100
500-50-50

0100
velocity [km/s]

150
counts [arbitrary units]

counts [arbitrary units]50-100200100

100-200[SII] 6716, PA=42.2 deg, 2009 02 10150

150
counts [arbitrary units]-200-300-500

-700

0-100

-50-100-100-100

0.30
0.25

0.30
0.25

0.35

0.20

0.20

0.25

0.15

0.15

0.20

90.05-0.00
-0.05
-0.10
-0.15

0.10
0.05
-0.00
-0.05
-0.10
-0.15

-0.20

-200

-100

0100
velocity [km/s]

200[SII] 6731, PA=3.1 deg, 2009 01 15

0.10
0.05
-0.00
-0.05
-0.10
-0.20

-0.25
-0.30
-300

300

-200

-100

0100velocity [km/s]

200

-0.25
-0.30
-300

300

[SII] 6731, PA=10.4 deg, 2008 03 19250

90.15

-0.15

-0.20

-0.25
-0.30
-300

-200

-100

0100
velocity [km/s]

200300[SII] 6731, PA=42.2 deg, 2009 02 10250Fig. 2. Emission lines of Ca II λ8498 (top row) and O I λ8446 (bottom row) in UVES spectra of ISO 143 at different observing times

150

counts [arbitrary units]

150

counts [arbitrary units]Mar. 2008, Jan. 2009, and Feb. 2009 in the order of increasing slit PA after continuum subtraction. The flux is given in arbitrary
V. Joergens, T.200Kopytova, A. Pohl: Discovery of an
outflow of the very low-mass star ISOin
143
100
units.
Gaussian fitting shows that the Ca II line can be decomposed into three components: (i) a narrow one centered close to zero200
counts [arbitrary units]

offset [arcseconds]

0.10

offset [arcseconds]

offset [arcseconds]

ISO143, spec3 [SII]6716
0.30

150

Table 2. Observed emission lines of ISO 143.
10050
0100

50
0velocity (probably chromospheric, green dotted line), (ii) a broader blue-shifted one (possibly produced in a wind, blue dotted line),and (iii) a very broad red-shifted one (possibly produced in magnetospheric infall, red dotted line). The pink dashed line is the sumof the Gaussian functions. The O I line can be fitted by a single red-shifted component in the two spectra from 2009 and by a blueand a red-shifted component in the spectrum from 2008 (the pink dashed line denotes here the sum of the two Gaussian functions).

500-50-50

lineslit PAdate

blue component

-50

-100
0.30
0.25

-100
0.30
0.25

green component

red component

-100

V

FWHM

EW

V 0.300.25[km/s][km/s][Å]

0.15[km/s]

FWHM

EW

VFWHM

EW

[km/s][Å][km/s][km/s]

[Å]

...
...
...

...
...
...

40.8
41.9
49.8

27.3
28.6
30.8

-0.2
-0.2
-0.2-0.30[S II]-200 -100 3.1
200901
15 -0.30-300 . . -200.
. .0 . 100 . 200. . 300 . . .-0.30-300 -200. . . -100 0 . . . 100 44.2
31.7
-300
0100
200
300
-100
200
300
[km/s]
velocity [km/s]
...
...
...
...
. . . velocity .[km/s]
..
44.5
26.7
(6730.82 Å) velocity
10.4
2008 03 19
42.2 analysis
2009 of02spectral
10 lines. . . of ISO 143. . . for three. . different.
. .observing.
. . . and slit
. . . PAs. Top
44.6row: photo32.5
Fig. 1. Spectro-astrometric
times

-0.4
-0.5
-0.4

sphericHe
line
as a test 2009
for artifacts,
FEL .ofof [S II] -0.4
λ6731. For. .each
I K I λ76993.1
01 15 middle. . row:.
. . [S II] λ6716,. . . bottom-0.5row: FEL
34.5. case, .we..
display the line profiles in the top panels, which are the average of 8 pixel rows in the spatial direction centered on the continuum. . . plots in. . .the bottom. . .panels,-2.3
26.2. . velocity...
(7065.19Å) subtraction,
10.4 and200803 19
aftercontinuum
the spectro-astrometric
which show
the spatial-0.5
offset vs.. radial
42.2asterisks)
2009...
. . . spectral. . . line (red2.4 squares).28.1.
.3.
of the continuum (blackand02of10
the continuum
subtracted
Velocities-0.5
are given. .relative
to .thestellar rest velocity V0 of ISO 143.

...
...
...

0.10

0.20

[deg]

0.05

-0.00
[S II]-0.05(6716.44Å)
-0.10
-0.15
-0.20

3.1
10.4
42.2

0.15
offset [arcseconds]

offset [arcseconds]

0.15

0.10

0.20

0.05

2009 01 15 -0.00 . . .
-0.05
2008 03 19 -0.10 . . .
...
2009 02 10 -0.15
-0.20

-0.25

...
...
...

...
...
...

offset [arcseconds]

0.20

0.10
0.05

. . .-0.00-0.05. . .-0.10. . .-0.15
-0.20

-0.25

-0.25

OI
(8446.36 Å)

3.1
10.4
42.2

2009 01 15
2008 03 19
2009 02 10

...
-42.1
...

...
61.3
...

...
-1.5
...

...
...
...

...
...
...

...
...
...

8.8
13.5
18.8

120.2
106.1
121.2

-3.7
-2.1
-5.5

Ca II
(8498.02 Å)

3.1
10.4
42.2

2009 01 15
2008 03 19
2009 02 10-1.0
-36.3
-18.4

60.0
51.1
41.4

-0.9
-0.6
-0.6

6.6
-1.3
5.9

8.5
20.9
20.2

-0.1
-0.5
-0.7

42.0
62.8
25.7

164.8
163.6
94.1

-1.7
-0.6
-4.1

Notes. The listed entries are: line with laboratory wavelength, slit PA,
observing date, and for each individual component the velocity at theline peak, the FWHM, and EW. The laboratory wavelengths are takenfrom the NIST database (http://physics.nist.gov/asd3, Ralchenko et al.
2011). The epochs are listed in the order of increasing slit PA, as in
Table 3, for clarity.

5・The simulation of molecular clouds formation in the Milky Way	

S.A. Khoperskov, E.O. Vasiliev, A.M. Sobolev and A.V. Khoperskov
ー銀河系の分子雲形成を3D流体計算でシミュレートをした
ーー水素分子化学反応、冷却過程、加熱過程を考慮
ーー広域の重力ポテンシャルは星バルジ、２つと４つの腕構造、星ディスク、ダークハローで与え、ガス成分の自己重力を考慮したーーこのモデルで腕のガス雲は、share and wiggle不安定星で形成され、t>100Myr後に分子雲となるーーt~100-300Myrで、分子雲は階層構造を形成し、100pcかそれ以上の大きさで密集するーーシミュレートで得られた分子雲の物理的特性を解析し、mass-spectrumの用なʻmass-sizeʻ関係と速度分散の統計的な分布が、銀河系で観測されているものと近いを示す
ーーシミュレーションで得られたガスの分布のl-v(銀経ー視線速度)図は、観測されたものと似ていて、銀河系の分子リングに似ている外観を持った構造を示す
ーーこのシミュレーションでこの構造が見られたことは、腕(~3-4pc)とバーからの放射の重ね合わせで説明できる

・Protostellar Accretion Flows Destabilized by Magnetic Flux Redistribution	

Ruben Krasnopolsky, Ruben, Zhi-Yun Li and Hsien Shang
ー磁場を含めた星形成の3Dシミュレーションーー磁場がすべて中心星に引きづり込まれると、観測されている値よりも大きくなってしまうʻ磁束問題ʼ
ーーこれは原理的にnon-ideal MHD効果を通じて経穴することができるーー(軸対象な)二次元計算で、ambipolar diﬀusionにより磁束を外に輸送することができる
ーこのような軸対象な原始星降着流を、3D計算すると方位角方向に磁気交換不安定星のため安定でないことを示す
ーーこの不安定星は中心に入る物質からの磁束の再分配により駆動されているーーそれは、星形成のprestellar段階から原始星の質量降着段階への移行時の発達を開始するーー後の段階で、以前に想定されていたよりも無秩序であるフィラメント上の降着流になる
ーー移流による磁束の外への効率的な輸送は、半径の小さいところで磁場の強度は下げ、回転円盤の形成
ーー＝＞でも、我々の3D計算では円盤は形成できなかったーーー原始星降着流は磁場再配分の不安定星で形成されているーーーこのような環境下で円盤はどうできるか不明である（できない）