The 6 67 hour period cco in rcw 103 a descendant of thorne zytkow object
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The 6.67 hour period CCO in RCW 103: a descendant of Thorne-Zytkow object?. X. W. Liu, R. X. Xu, G. J. Qiao, J. L. Han, Z. W. Han, and X. D. Li, submitted to ApJ arXiv:1207.4687v1 [astro-ph.HE]. XiongWei Liu (Peking University) 刘雄伟 16 Aug. 2012, Urumchi. Background

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The 6.67 hour period CCO in RCW 103: a descendant of Thorne-Zytkow object?

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The 6 67 hour period cco in rcw 103 a descendant of thorne zytkow object

The 6.67 hour period CCO in RCW 103: a descendant of Thorne-Zytkow object?

X. W. Liu, R. X. Xu, G. J. Qiao, J. L. Han, Z. W. Han, and X. D. Li, submitted to ApJ

arXiv:1207.4687v1 [astro-ph.HE]

XiongWei Liu (Peking University)

刘雄伟

16 Aug. 2012, Urumchi


The 6 67 hour period cco in rcw 103 a descendant of thorne zytkow object

  • Background

    The 6.67h period X-ray source in RCW 103

  • From TZO to extremely long period CCO

    What is a TZO?

    How to spin down?

    Why looks like a CCO?

  • Discussion


Background the 6 67h period x ray source in rcw 103

BackgroundThe 6.67h period X-ray source in RCW 103


The 6 67h period x ray source in rcw 103

The 6.67h period X-ray source in RCW 103

1E161348-5055

(Tuohy, 1980)

soft x-ray

~1033 – 1035 erg s-1,

no radio or optical counterpart

SNR RCW 103

~2 kyr (Carter, 1997)

~3.3 kpc


The 6 67h period x ray source in rcw 1031

The 6.67h period X-ray source in RCW 103

6.67-hour periodicity modulation (2006, De Luca)

any other periodicities with P >12 ms are excluded with high confidence


The 6 67h period x ray source in rcw 1032

The 6.67h period X-ray source in RCW 103

Long-term flux variability (2006, De Luca)


The 6 67h period x ray source in rcw 1033

The 6.67h period X-ray source in RCW 103

Period derivative(2011, Esposito)


The 6 67h period x ray source in rcw 1034

The 6.67h period X-ray source in RCW 103

Candidate 1: Orbit period of a binary?

Neutron star + low mass MS star

(2006, De Luca)

MNS=1.4 M⊙, Porbit=6.67h

black line: Mcom = 0.4 M⊙, e = 0.2;

red line: Mcom = 0.2 M⊙, e = 0.5.

wind velocity: 300 km s-1.

Problems:

How could the company star survive from the supernova explosion and escape the observations?

Why didn’t find the spin period?


The 6 67h period x ray source in rcw 1035

The 6.67h period X-ray source in RCW 103

Candidate 2: Magnetar with a fallback disk?

(2006, De Luca)

magnetic field: 5×1015 G

disc mass: 3×10-5 M⊙

birth period: 0.3 s

Problems:

Why doesn’t like other “magnetars”? (P: 2~12s)

AXP 0142, Disk (Wang 2006)

SGR 0418+5729, Disk spin-down (Alpar 2011)


From tzo to extremely long period cco what is a tzo how to spin down why looks like a cco

From TZO to extremely long period CCOWhat is a TZO?How to spin down?Why looks like a CCO?

Candidate 3:


What is a tzo

What is a TZO?

Thorne-Zytkow Object (TZO) (Thorne & Zytkow, 1977):

A massive star with a degenerate neutron core

Structure of a TZO

20-200 TZOs existing in the Galaxy (Podsiadlowski et al. 1995),

But identified none.


How to spin down

How to spin down?

Philipp et al. 1995, MNRAS

In the steady-burning phase

Slowly spin-down

In the neutrino runaway phase

Spin-up to ~10ms

But they ignored the interaction between envelope and magnetosphere, and did not consider the out-flow


How to spin down1

How to spin down?

Qualitatively:

When the envelope particals go in to the core (inflow),

they are accelerated by the magnetosphere;

When some of them go out (ourflow),

they take away angular momentum from the core.

Notes:

it is radiation press dominanted

it is not disk accretion

there is no Alphen radius


How to spin down2

How to spin down?

Quantitatively:

Structure of the convection envelope

Mass conservation:

Boundary conditions:

Hypothesis:

(flow structure)


How to spin down3

How to spin down?

Quantitatively:

Interaction between magnetosphere and particals,

rotational velocity:


How to spin down4

How to spin down?

Quantitatively:

Conservation of angular momentum:


How to spin down5

How to spin down?

Quantitatively:

Main results:

  • The spin evolution of the compact core in a TZ˙O with different core parameters and same model parameters


How to spin down6

How to spin down?

Quantitatively:

Main results:

  • The spin evolution of the compact core in a TZ˙O with different model parameters and same core parameters


Why looks like a cco

Why looks like a CCO?

  • Case a: About 2000 years ago, the more massive star of a binary collapsed in a supernova explosion, which produced RCW 103 and a compact star. The compact star embedded in the companion MSS and formed a TZO. The core spun-down to the co-rotational period (6.67 hr) with the envelop within 2000 years, when a burst destroyed the envelope (e.g., due to a phase transition of its crust, or other processes such as thermal nuclear explosion). As a result, the envelope mixed together with the supernova remnant RCW 103, and the core (1E1613) became a CCO.

  • Case b: More than 2000 years ago, a neutron star embedded in or swallowed by its companion star and formed a TZO. About 2000 years ago, a powerful burst (the whole neutron star occurred a phase transition or a quark-nova) took place , when it has spun-down to 6.67 hr and the previous supernova remnant has faded away. The burst destroyed the TZO envelope and formed an analogous supernova remnant, i.e. RCW 103. The young quark star (1E1613) became a CCO.


Summary and discussion

Summary and discussion

  • The core of a TZO would spin down quickly to the corotate period with envelope braked by the interaction between the envelope and magnetosphere;

  • The core could manifest as a long period isolated compact star if a energetic burst destroy the envelope;

  • The CCO in RCW 103, 1E1613, might be a descendant of a disrupted TZO.

  • It also could be one of the possible origin of the extremely long period objects in X-ray binaries. Such as the ~2.7 hour period X-ray source in 2S 0114+65 and the ~1.5 hour period X-ray source in 4U 2206+54.

Thanks!


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