Pinpointing
This presentation is the property of its rightful owner.
Sponsored Links
1 / 35

Pinpointing a stellar X-ray flare using XMM-Newton and VLT/UVES PowerPoint PPT Presentation


  • 80 Views
  • Uploaded on
  • Presentation posted in: General

Pinpointing a stellar X-ray flare using XMM-Newton and VLT/UVES. J.U. Ness J. Robrade J.H.M.M. Schmitt. Uwe Wolter Hamburger Sternwarte May 2008. 2006 October 14. 2006 October 15. Speedy Mic‘s rotation. XMM orbit 1254. VLT visibility. XMM observations.

Download Presentation

Pinpointing a stellar X-ray flare using XMM-Newton and VLT/UVES

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Pinpointing a stellar X-ray flare using XMM-Newton and VLT/UVES

J.U.Ness

J.Robrade

J.H.M.M.Schmitt

Uwe Wolter

Hamburger Sternwarte

May 2008


Pinpointing a stellar x ray flare using xmm newton and vlt uves

2006 October 14

2006 October 15

Speedy Mic‘s rotation

XMM orbit 1254

VLT visibility

XMM observations

The observations: Synchronizing orbits, night-time visibility, instrument schedules, …

 50 ks XMM-Newton data + 142 VLT/UVES spectra


Pinpointing a stellar x ray flare using xmm newton and vlt uves

The target: Speedy Mic (BO Mic)A single K-dwarf - ultrafast and highly active

P = 0.380 ± 0.004 d

( Cutispoto et al. 1997 )

v sini = 132 ± 2 km/s

( Wolter et al. 2005 )

A giant flare (E > 1036 erg)

Kürster 1994

DSS, d ≈ 0.0002“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

CaKEquivalent width

EPIC-pn

A „moderate“ flare in X-rays and optical

≈ 4.5 hours

Rotation Phase

Wolter et al. 2008

Total flare energy in soft X-rays:~ 1034 erg


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Chromospheric emissionRotational Modulation

Ca II Kλ3933 Ǻ

Wolter & Schmitt 2005


Pinpointing a stellar x ray flare using xmm newton and vlt uves

A

2006 flare

C

C

9.4 h

B

B

Rotation Phase

A

1.7 Å@ 4000 Å

Wavelength

„unsharp masked“

Wavelength

Rotation Phase

Evolution of

CaIIK

Line Profiles


Pinpointing a stellar x ray flare using xmm newton and vlt uves

log T [K]

0.5 · log EM [cm-3]

Flare heating and cooling

 Loop half length

240,000 km

≈ 0.4 R*

Wolter, Robrade et al. 2008; Reale et al.2004


Pinpointing a stellar x ray flare using xmm newton and vlt uves

<<<<<<<<<<<

A flare in a context

Phase 4.2

Phase 3.9

Wolter et al. 2008

ESO PR 53-2007

Phase 4.6


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Summary

  • X-ray flare sites can be localized by simultaneous optical/UV Doppler imaging

  • Flare sites are not necessarily conspicuous otherwise

„ … on returning within

60 seconds was mortified

to find that it was already

much … enfeebled.“

(R. Carringon 1859, MNRAS XX)

Wolter, Robrade, Schmitt & Ness 2008, A&A 478, L12ESO Press Release 53/07 „Speedy Mic‘s Photograph“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Appendix


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Outlook: Chromospheric heating events

Rotation Phase

He I 5875, Ca II 3933 and XMM-pn at 300 s resolution


Pinpointing a stellar x ray flare using xmm newton and vlt uves

A „solar-like“ spectrum

Hα6562.81 Ǻ

Na D25889.97 Ǻ

Na D15895.94 Ǻ

Hβ4861.34 Ǻ

Ca II K 3933.68 Ǻ

Ca II H 3968.49 Ǻ

(NOAO)

Arcturus (α Boo, K1 III, Teff ≈ 5200 K )


Pinpointing a stellar x ray flare using xmm newton and vlt uves

The Doppler imaging principle:

Line profiles → spatial information

e.g. Deutsch 1958, Vogt & Penrod 1983, Wolter 2004


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Speedy Mic vs. SunUltrafast rotation and high activity

Sun

SpeedyMic

Valenti 2001, Sterzig & Schmitt 1997, Cardini et al. 2007, Balihunas et al. 1995


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Lost and found


Pinpointing a stellar x ray flare using xmm newton and vlt uves

„Ultrafast rotators“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

„Ultrafast rotators“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

BO „Speedy“ Mic in 2002

(HD 197890)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Aug 2

„6400 Å“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Aug 7

„6400 Å“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Photometry 2002

(SAAO)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

The Prominences …


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Evolution of Hα(Aug 2)

line profiles


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Hα(Aug 2)

CaII K (Aug 2)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

„A densely packed prominence system beyond co-rotation“

Hα(Aug 2)

Hα(July 19)

r ≈ 5 ± 1.5 R*

r = 3.5 ± 0.6 R*

Rk = 1.95 ± 0.07 R*

Dunstone et al. 2006 (adapted)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

RXJ 1508.6±4423 („post T Tauri“)

Hα emission

AB Dor

Hα absorption transients

Stellar prominences

Donati et al. 2000

Collier Cameron & Robinson 1989


Pinpointing a stellar x ray flare using xmm newton and vlt uves

The Plage(s) …


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Localizing one stellar plage

φ = 112° θ = 130°

CaIIK(Aug 2)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

„Localizing one (?) stellar plage“

(Aug 7)

CaIIK(Aug 2)

φ = 72°

θ = 99°

φ = 112°

θ = 130°


Pinpointing a stellar x ray flare using xmm newton and vlt uves

The Flare …


Pinpointing a stellar x ray flare using xmm newton and vlt uves

APOD April 2006

„Astronomers love stars …“

(Zirrin 1988)

„… and we have a fine one right near us.“

DOT


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Hα pre-flare

Hα flare (21:06 UT)

The 1993 March 6 solar flare

Johns-Krull et al. 1997


Pinpointing a stellar x ray flare using xmm newton and vlt uves

GOES „soft X-ray“

20:23

„Unfortunately, the observer was eating lunch when the flare began.“


Pinpointing a stellar x ray flare using xmm newton and vlt uves

Solar flare Hα profiles

(near max.)


Pinpointing a stellar x ray flare using xmm newton and vlt uves

„after peak“

Another solar flare

(Hα – 0.5 Å)

higher density

„raining down“

Zirrin 1988 (BBSO)


  • Login