The Chandra Delta Ori Large Project: Occultation Measurements Of The Shocked Gas In The Nearest Eclipsing O-Star Binary!

250

200

150

100

50

0

Coun

ts/b

in

252015105

Wavelength (Angstroms)

OVIIIFe

XVIII

FeXV

III

FeXV

IIIFe

XVIII

NeIX

NeX

MgX

II

MgX

I

NeX

SiXI

IISi

XIV

OVIIFe X

XIII

MgX

I

SXV

Fe X

VIII

OVIII

OVII

N VI

ISiXI

II

SXVI

NeIX

NeIX

OVII

OVII

Fe X

XIFe

XVI

I

Fe X

XNeX

Ne IX

Fe X

XIII

Fe X

XIII

200

150

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50

0

Coun

ts/b

in

252015105Wavelength (Angstrom)

Combined Data (all HEG and MEG) 3 component APED model w/line broadening

(xaped(1)+xaped(2))*TBabs(3)+xaped(4)*TBabs(5) idx param tie-to freeze value min max 1 xaped(1).norm 0 0 0.004548259 0 10 2 xaped(1).temperature 0 0 3334460 1000000 1e+09 3 xaped(1).density 0 0 5.304466e+12 1000000 1e+25 4 xaped(1).vturb 0 0 1143.372 0 3000 5 xaped(1).redshift 0 1 0 -1 1 6 xaped(1).metal_abund 0 1 1 0 10 7 xaped(2).norm 0 0 0.02328348 0 100 8 xaped(2).temperature 0 0 1246984 100000 1e+09 9 xaped(2).density 0 1 1e+23 1000000 1e+25 10 xaped(2).vturb 0 1 1000 0 3000 11 xaped(2).redshift 0 1 0 -1 1 12 xaped(2).metal_abund 0 1 1 0 10 13 TBabs(3).nH 0 0 0.1444799 0 100000 10^22 14 xaped(4).norm 0 0 0.00133482 0 100 15 xaped(4).temperature 0 0 9107113 100000 1e+09 16 xaped(4).density 0 1 1e+23 1000000 1e+25 17 xaped(4).vturb 0 0 685.5451 0 2000 18 xaped(4).redshift 0 1 0 -1 1 19 xaped(4).metal_abund 0 1 1 0 10 20 TBabs(5).nH 0 0 0.2415301 0 100000 10^22

8x10-4

6

4

2

0

Coun

t Ra

te (

cts

s-1 b

in-1

)

9.59.49.39.29.19.0

Wavelength (Angstrom)

Mg

XI (

w)

Mg

XI (

x+y)

Mg

XI (

z)

14567_rate_smth 14569_rate_smth 14570_rate_smth 14568_rate_smth

8x10-4

6

4

2

0

Coun

t Ra

te (

cts

s-1 b

in-1

)

6.96.86.76.66.5

Wavelength (Angstrom)

Si X

III (w

)

Si X

III (x

+y)

Si X

III (z

)

14567_rate_smth 14569_rate_smth 14570_rate_smth 14568_rate_smth

0.0008

0.0006

0.0004

0.0002

0.0000

Coun

t Ra

te (

cts

s-1 b

in-1

)

12.2512.2012.1512.1012.0512.00

Wavelength (Angstrom)

-2000 0 2000

Velocity (km s-1)

Ne X

14567_rate_smth 14569_rate_smth 14570_rate_smth 14568_rate_smth

� Ori Parameters

Stellar ParametersStar Aa1 Star Aa2

Sp. Type O9.5IIR(R�) 17 7M(M�) 25 10Teff

32900log g

eff

3.12

M(M� yr�1) 10�6 10�7

V1 2000 1500System ParametersP (days) 5.732436e 0.09i 67�

! 148�

Tperiastron

(MJD) 54002.205± 0.060

Chandra VLP Observing LogObsID 14567 14568 14569 14570

Date Start 2012-12-19T16:54 2012-12-27T03:53 2012-12-22T06:06 2012-12-24T13:14Phase Start 396.604 397.905 397.049 397.450Date End 2012-12-21T01:48 2012-12-28T14:50 2012-12-23T16:12 2012-12-26T00:23Phase End 396.844 398.159 397.297 397.705Duration (Days) 1.34 1.46 1.42 1.46Exposure (ksec) 115 122 119.3 122.5

1

5.36

5.44

5.52

mag

4735.0 4738.0 4741.0 4744.0 4747.0 4750.0 4753.0HJD 2451545 + days

5.36

5.44

5.52

mag

8

16

24

po

ints

bin

�1

20

40

60

po

ints

bin

�1

Summary!

In December 2012 Delta Ori was observed by Chandra using the HETGS for a total of 478 ksec spanning an entire orbital cycle. Simultaneous photometric data with MOST was obtained. These observations show in the optical and X-ray photometry and X-ray emission line spectrum which are not strictly phase-locked, along with phase-locked variabilty.!

See Poster by Nichols et al. for a summary of the variability analysis.!

Introduction!Delta Ori is the nearest massive, single-lined eclipsing binary (O9.5 II + B0.5III). As such it serves as a fundamental calibrator of the mass-radius-luminosity relation in the upper HR diagram. It is also the only eclipsing O-type binary system which is bright enough to be observable with the CHANDRA gratings in a reasonable exposure. Studies of resolved X-ray line complexes provide tracers of wind mass loss rate and clumpiness; occultation by the X-ray dark companion of the line emitting region can provide direct spatial information on the location of the X-ray emitting gas produced by shocks embedded in the wind of the primary star. We obtained phase-resolved spectra with Chandra in order to determine the level of phase-dependent vs. secular variability in the shocked wind. Along with the Chandra observations we obtained simultaneous photometry from space with the Canadian MOST satellite to help understand the relation between X-ray and photospheric variability.

• Unusually large variations in the X-ray lightcurve!

• Significant non-phase-locked photometric variations: pulsations?!

left: combined 478 ksec HETG spectrum of Delta Ori. right: simple 2 component fit to the combined spectrum, which recovers the line spectrum and continuum and which shows the suppression of the forbidden lines of OVII and Ne IX. !

He-like Lines: Mg XI and Si XIII! H-like Lines: Ne X and O VIII!

0.0006

0.0005

0.0004

0.0003

0.0002

0.0001

0.0000

Coun

t Rat

e (c

ts s

-1 b

in-1

)

19.1019.0018.9018.80

Wavelength (Angstrom)

-2000 -1000 0 1000 2000Velocity (km s-1)

OVIII

14567_rate_smth (0.60-0.84) 14569_rate_smth (0.05-0.30) 14570_rate_smth (0.45-0.71) 14568_rate_smth (0.90-1.16)

Michael F. Corcoran (USRA & NASA/GSFC), Joy Nichols (SAO), Yael Naze & Gregor Rauw (U. Liege), Andrew Pollock (ESA), Anthony Moffat & Noel Richardson (U. Montreal), Nancy Evans (SAO), Kenji Hamaguchi (UMBC & NASA/GSFC), Lida Oskinova & W.-R. Hamann (Potsdam), Ted Gull (NASA/GSFC), Rico Ignace & Tabetha Hole (East Tennessee State), Rosina Iping (UMCP), Nolan Walborn (STScI), Jennifer Hoffman & Jamie Lomax (U. Denver), Wayne Waldron (Eureka Scientific), Stan Owocki (U. Delaware), Jesus Maiz-Apellaniz (IA Andalucia-CSIC), Maurice Leutenegger (UMBC & NASA/GSFC), Tabetha Hole (Weber), Ken Gayley (U. Iowa), Chris Russell (JSPS/Hokkai-Gakuen University) and the MOST team

Schematic of the orbit of the secondary star around the primary in Delta Ori. The bars show the estimate of the formation regions of Ne IX, Mg XI and O VII from Miller et al. (2002 ApJ, 577, 951).

The Delta Ori HETGS spectrum:!

X-ray and Optical Variability!

Delta Ori (Mintaka)

Chandra Zeroth-Order X-ray lightcurve (4-30 Angstroms) MOST lightcurve (3500-7000 Angstroms, courtesy MOST team). The vertical lines show the timing of the Chandra observations.

1457

0

1456

7

1456

9

1456

8

� Ori Parameters

Stellar ParametersStar Aa1 Star Aa2

Sp. Type O9.5II B0.5 IIIR(R�) 17 7M(M�) 25 10Teff

(K) 32900 24000Lbol

(105L�) 2.2 0.2log g

eff

3.38 3.76

M(M� yr�1) 10�6 10�7

V1 2000 1500System ParametersP (days) 5.732436e 0.09i 67�

! 148�

Tperiastron

(MJD) 54002.205± 0.060

Chandra VLP Observing LogObsID 14567 14568 14569 14570

Date Start 2012-12-19T16:54 2012-12-27T03:53 2012-12-22T06:06 2012-12-24T13:14Phase Start 396.604 397.905 397.049 397.450Date End 2012-12-21T01:48 2012-12-28T14:50 2012-12-23T16:12 2012-12-26T00:23Phase End 396.844 398.159 397.297 397.705Duration (Days) 1.34 1.46 1.42 1.46Exposure (ksec) 115 122 119.3 122.5

1

https://ntrs.nasa.gov/search.jsp?R=20140010267 2020-06-20T10:14:15+00:00Z