Solar vicinity, closeby young isolated NSs, and tests of cooling curves

1
Solar vicinity, close-by young isolated NSs,and
tests of cooling curves

• Sergei Popov
• (Sternberg Astronomical Institute)
• Co-authors H.Grigorian, R. Turolla, D. Blaschke

ECT, Trento, September 14, 2005
2
Plan of the talk

• Intro. Close-by NSs
• Age-Distance diagram
• Solar vicinity. Stars
• Spatial distribution
• Mass spectrum
• Two tests of cooling
• Brightness constraint
• Sensitivity of two tests
• Final conclusions

3
Isolated neutron stars population in the
Galaxy and at the backyard

• INSs appear in many flavours
• Radio pulsars
• AXPs
• SGRs
• CCOs
• RINSs

Note a recent discovery by Lyne et al.
(submited to Nature, see later)

• Local population of young NSs
• is different (selection)
• Radio pulsars
• Geminga
• RINSs

4
Close-by radioquiet NSs

• Discovery Walter et al. (1996)
• Proper motion and distance Kaplan et al.
• No pulsations
• Thermal spectrum
• Later on six brothers

RX J1856.5-3754
5
Magnificent Seven
Radioquiet (?) Close-by Thermal emission Long
periods
6
Population of close-by young NSs

• Magnificent seven
• Geminga and 3EG J18535918
• Four radio pulsars with thermal emission
  (B0833-45 B065614 B1055-52 B192910)
• Seven older radio pulsars, without detected
  thermal emission.

7
Age-distance diagram
A toy-model a local sphere (R300 pc) and a flat
disk. Rate of NS formation in the sphere is 235
Myr-1 kpc-3 (26-27 NS in Myr in the whole
sphere). Rate in the disc is 10 Myr-1 kpc-2 (280
NS in Myr up to 3 kpc).
(astro-ph/0407370)
8
More realistic age-dist. diagram
Initial distribution from Popov et al.
2005. Spatial evolution is not followed. For
the line of visibility (solid line in the
middle) I assume the limiting flux 10-12 erg s-1
cm-2 and masses are lt1.35 (Yakovlev et al.
curves).
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Realistic age-distance diagram
Realistic initial distribution. Spatial
evolution is taken into account. The line of
visibility is drawn as the dotted line. Five
curves correspond to 1, 4 , 13, 20 and 100 NSs.
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Solar vicinity

• Solar neighborhood is not a typical region of our
  Galaxy
• Gould Belt
• R300-500 pc
• Age 30-50 Myrs
• 20-30 SN per Myr (Grenier 2000)
• The Local Bubble
• Up to six SN in a few Myrs

11
The Gould Belt

• Poppel (1997)
• R300 500 pc
• Age 30-50 Myrs
• Center at 150 pc from the Sun
• Inclined respect to the galactic plane at 20
  degrees
• 2/3 massive stars in 600 pc belong to the Belt

12
Distribution of open clusters
(Piskunov et al. astro-ph/0508575)
13
Surface density of open clusters
(Piskunov et al.)
14
Spatial distribution of close-by open clusters in
3D
Grey contours show projected density distribution
of young (log Tlt7.9) clusters.
(Piskunov et al.)
15
Clusters and absorption
Triangles Gould Belt clusters.
(Piskunov et al.)
16
Spatial distribution
More than ½ are in /- 12 degrees from the
galactic plane. 19 outside /- 30o 12 outside
/- 40o
(Popov et al. 2005 ApSS 299, 117)
Lyne et al. reported transient dim radio sources
with possible periods about seconds in the
galactic plane discovered in the Parkes
survey (talk by A. Lyne in Amsterdam, august
2005 subm. to Nature).
Shall we expect also Lynes objects from the
Belt???? YES!!! And they even have to be brighter
(as they are closer). The problem low
dispersion.
17
Mass spectrum of NSs

• Mass spectrum of local young NSs can be different
  from the general one (in the Galaxy)
• Hipparcos data on near-by massive stars
• Progenitor vs NS mass Timmes et al. (1996)
  Woosley et al. (2002)

(masses of secondary objects in NSNS)
astro-ph/0305599
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Two tests
Age Temperature
Log N Log S
19
Standard test temperature vs. age
Kaminker et al. (2001)
20
Log N Log S
calculations
-3/2 sphere number r3
flux r-2
Log of the number of sources brighter than the
given flux
-1 disc number r2 flux
r-2
Log of flux (or number counts)
21
Log N Log S as an additional test

• Standard test Age Temperature
• Sensitive to ages lt105 years
• Uncertain age and temperature
• Non-uniform sample
• Log N Log S
• Sensitive to ages gt105 years
• (when applied to close-by NSs)
• Definite N (number) and S (flux)
• Uniform sample
• Two test are perfect together!!!

astro-ph/0411618
22
List of models (Blaschke et al. 2004)
Pions Crust Gaps

• Blaschke et al. used 16 sets of cooling curves.
• They were different in three main respects
• Absence or presence of pion condensate
• Different gaps for superfluid protons and
  neutrons
• Different Ts-Tin

• Model I. Yes C A
• Model II. No D B
• Model III. Yes C B
• Model IV. No C B
• Model V. Yes D B
• Model VI. No E B
• Model VII. Yes C B
• Model VIII.Yes C B
• Model IX. No C A

23
Model I

• Pions.
• Gaps from Takatsuka Tamagaki (2004)
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
24
Model II

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Tsuruta (1979)

Cannot reproduce observed Log N Log S
25
Model III

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
26
Model IV

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
27
Model V

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Tsuruta (1979)

Cannot reproduce observed Log N Log S
28
Model VI

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Yakovlev et al. (2004)

Cannot reproduce observed Log N Log S
29
Model VII

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1.
• 1P0 proton gap suppressed by 0.5
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
30
Model VIII

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1. 1P0 proton gap suppressed by
  0.2 and 1P0 neutron gap suppressed by 0.5.
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
31
Model IX

• No Pions
• Gaps from Takatsuka Tamagaki (2004)
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
32
HOORAY!!!!
Log N Log S can select models!!!!! Only three
(or even one!) passed the second
test! .still is it possible just to
update the
temperature-age test??? May be Log N Log S is
not necessary? Lets try!!!!
33
Brightness constraint

• Effects of the crust (envelope)
• Fitting the crust it is possible to fulfill the
  T-t test
• but not the second test Log N Log S
  !!!

(H. Grigorian astro-ph/0507052)
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Sensitivity of Log N Log S

• Log N Log S is very sensitive to gaps
• Log N Log S is not sensitive to the crust if it
  is applied to relatively old objects (gt104-5 yrs)
• Log N Log S is not very sensitive to presence
  or absence of pions

Model I (YCA) Model II (NDB) Model III
(YCB) Model IV (NCB) Model V (YDB) Model
VI (NEB) Model VII(YCB) Model VIII (YCB)
Model IX (NCA)
We conclude that the two test complement each
other
35
THATS ALL. THANK YOU!
36
Resume

• We live in a very interesting region of the Milky
  Way!
• Log N Log S test can include NSs with
• unknown ages, so additional sources
• (like the Magnificent Seven) can be used
• to test cooling curves
• Two tests (LogNLogS and Age-Temperature) are
  perfect together.

37
Radio detection
Malofeev et al. (2005) reported detection of
1RXS J1308.6212708 (RBS 1223) in the
low-frequency band (60-110 MHz) with the radio
telescope in Pushchino.
(back)
38
Evolution of NS spin magnetic field
Ejector ? Propeller ? Accretor ? Georotator
1 spin-down 2 passage through a molecular
cloud 3 magnetic field decay
astro-ph/0101031
Lipunov (1992)
39
Model I

• Pions.
• Gaps from Takatsuka Tamagaki (2004)
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
(back)
40
Model IX

• No Pions
• Gaps from Takatsuka Tamagaki (2004)
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
(back)
41
Model III

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
(back)
42
Model II

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Tsuruta (1979)

Cannot reproduce observed Log N Log S
(back)
43
Model IV

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
(back)
44
Model V

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Tsuruta (1979)

Cannot reproduce observed Log N Log S
(back)
45
Model VI

• No Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1
• Ts-Tin from Yakovlev et al. (2004)

Cannot reproduce observed Log N Log S
(back)
46
Model VII

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1.
• 1P0 proton gap suppressed by 0.5
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Cannot reproduce observed Log N Log S
(back)
47
Model VIII

• Pions
• Gaps from Yakovlev et al. (2004), 3P2 neutron gap
  suppressed by 0.1. 1P0 proton gap suppressed by
  0.2 and 1P0 neutron gap suppressed by 0.5.
• Ts-Tin from Blaschke, Grigorian, Voskresenky
  (2004)

Can reproduce observed Log N Log S
(back)
48
NSNS binaries
Pulsar Pulsar mass
Companion mass B191316 1.44
1.39 B212711C
1.35 1.36 B153412
1.33
1.35 J0737-3039 1.34
1.25 J1756-2251 1.40
1.18
(PSRcompanion)/2 J15184904
1.35 J1811-1736
1.30 J18292456
1.25
(David Nice, talk at Vancouver)
(Back)
49
P-Pdot for new transient sources
Lyne et al. 2005 Submitted to Nature (Im
thankful to Prof. Lyne for giving me an
opportunity to have a picture in advance)
Estimates show that there should be about
400 000 sources of this type in the Galaxy
(back)