Orbital evolution of compact Black-hole binaries and white dwarf binaries
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Orbital evolution of compact Black-hole binaries and white dwarf binaries. Astro-ph/0511760. Astro-ph/0510331. Wencong Chen. Astro-ph/0511760. Magnetic braking of Ap/Bp stars: application to compact BH X-ray binaries. 1.Introduction:. Conventional magnetic braking (MB):.

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Orbital evolution of compact Black-hole binaries and white dwarf binaries

Astro-ph/0511760

Astro-ph/0510331

Wencong Chen


Astro-ph/0511760 dwarf binaries

Magnetic braking of Ap/Bp stars: application to compact BH X-ray binaries

1.Introduction:

Conventional magnetic braking (MB):

radiative envelopes inoperative, Md<1.5 solar mass

Author’s suggestion:

Compact binaries with Ap & Bp stars

Irradiation driven stellar wind

Lead to significant MB


9 of 17 compact BH X-ray binaries: dwarf binaries

P<1d, Md<1 solar mass

Galactic:

1000 short period BH binaries (Wijers, 96; Romani, 98)

How to form short period and low donor mass BH binaries?

Intermediate mass (IM) star with Strong magnetic field, irradiation driven wind

A plausible AM loss mechanism

Produce short period low mass BH binaries


2. Assumptions and derivations: dwarf binaries

Assume wind corotates out to magnetospheric radius

Loss rate of AM due to MB:


2.1 estimate of the required wind loss rate dwarf binaries

Mass conservative

If adot<0


For a typical mass ratio dwarf binaries

Mass –radius relation of donor star


2.2 Irradiation driven winds dwarf binaries

Stellar wind was driven irradiation in compact binaries ( Ruderman 89)

Irradiation stellar wind loss rate

Wind driving parameter

maximum


2.3 analytic results for dwarf binaries

MB torque:

Total AM of system

Mass conservative and adot=0



3. BH binary populations dwarf binaries

Suggest part of IM star possess strong magnetic field (Ap,Bp stars)

New MB in strong field systems via irradiation induced stellar wind

Cause a subset of BH binaries to evolve to short periods

Assume Bs is a constant, even during mass loss

Use an updated version of Eggleton’s code

Initial conditions:


3.1 long and short period: population statistics dwarf binaries

Ap stars ~5% in A stars

Zero magnetic field: 0.2-0.4Gyr

Strong field: 10Gyr



4. Summary and conclusions dwarf binaries

New MB can cause BH binaries involving Ap/Bp donor stars to evolve to short periods (P<10hr)

BH binaries with IM donor star is reasonable than ones with low mass donor star

Author’s model is successful at reproducing the short periods and low donor mass

Shortcoming:

Calculative effective temperatures are significantly higher that for those of the observed donor stars.


Astro-ph/0510331 dwarf binaries

Detection of a period decrease in NN Ser with ULTRACAM: evidence for strong magnetic braking or an unseen companion

1.introduction:

CVs: white dwarf primary

low mass main sequence secondary

Main period distribution: 1.3-10 hours

Two major features:

Period gap 2-3 hours

period minimum 1.3 hour

Standard model


In this paper: dwarf binaries

Measure mid-eclipse timing

find period change

To calculate AM loss

Pdot~5*10^(-4) s /yr

Contamination of light curve by accretion process

So choose pre-CV NN ser

High time resolution of ULTRACAM ~0.15S

NN ser:

WD and M dwarf with ~0.15 solar mass

Deeply eclipsing >4.8mag, strong reflection effect ~0.6mag

Orbital period 0.13days


2. Analysis & results: dwarf binaries

A best fit linear ephemeris

A best fit quadratic ephemeris

Eclipse time

Rate of period decrease


The average rate of period change dwarf binaries

The current rate of period change


3. discussion- mechanisms for period changes: dwarf binaries

Applegate’s mechanism (92)

Presence of third body in a long orbit around binary

A genuine AM loss

3.1 Applegate’s mechanism

Gravitational coupling

Shape change of secondary

Change of quadrupole moment

Period change


3.2 dwarf binariesthird body

Light travel time variation leads to period change

0.0043 solar mass < M3 < 0.18 solar mass

30yr < P3 < 285 yr

A low mass companion could cause the observed changes in mid-eclipse timings


3.3 AM loss models dwarf binaries

1. Gravitational radiation

2. Standard MB

(Rappaport, 83)


3. Reduced MB dwarf binaries

(Sills, 2000)


4. conclusions: dwarf binaries

Two possible explanations:

Presence of a third body

Genuine AM loss: standard MB by Rappaport, no cut off

Reduced MB underestimate ~ 2 orders of magnitude


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