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OBSID:
29117
 Title:
After a Mega-Flare: Surface Magnetic Fields, Particle Ejection and Disk Ionization
Investigator:
Getman
 Observer:
Getman, Konstantin
 Phone:
814-4415876
 Email:
kug1@psu.edu
Target Name:
Orion Nebula Cluster
 Sequence Number:
201581
 Instrument:
ACIS-I
 Grating:
NONE
 SI Mode:
TE_006E6B
 Raster Scan:
N
 Annotated DOT:
DEC1123a

Proposal Number:
24200395
 Right Ascension:
83.8196
 Declination:
-5.39
 Status:
archived
 Start Date:
2023-12-18 04:53:32
Category:
STARS AND WD
 Type:
GO
 AO Cycle:
24
 Dither Flag:
Y
 Y Offset:
0
 Z Offset:
0
Est. Count Rate:
0.1
 Order-1 Count Rate:

 Exposure Time:
13
 Time Remaining:
12.092
 Reqd Start Time:

 Reqd Stop Time:
Period:

 Epoch:

 Start of Period:

 End of Period:

 PS Margin:

 PE Margin:

 Max Segments:
0

ACIS Mode:
TE
 Standard?:
No
 BEP Mode:
VF
On-Chip Summing?:
No
 Row Sum:

 Column Sum:

 Frame Time:
Subarray Mode:
NONE
 Starting Row:
0
 Row Count:
1023
 Subarray Frame Time:

Duty Cycle?:
No
 Cycle Count:
0
 Primary Exp Time:

 Secondary Exp Time:
Event Filter?:
No
 Filter Threshold:

 Filter Range:

 Bias Requested?:
No
 Bias Frequency:

 Bias After?:
No
 Spatial Window?:
No

Abstract:
The most powerful magnetic reconnection flares in normal stars occur during the pre-main sequence phase, and the greatest number of flares accessible to a single pointing of Chandra is the Orion Nebula Cluster. In this multi-telescope project, Chandra will repeatedly observe the ONC to identify mega-flares with enormous energies. These flares will trigger ground-based observations over the following days to: detect extended radio emission from mega-flare coronal mass ejections with the VLBA; test predictions of elevated surface magnetic field strengths by Zeeman infrared spectroscopy; and study the rise and fall of ionization in a protoplanetary disk following a stellar mega-flare with H13CO+ emission using ALMA.

Remarks:
We propose to obtain unique observations with the VLBA up to three times per year (three 8-hour tracks), if they can be scheduled either simultaneously or within 10 days of the Chandra observations. If they cannot be scheduled within this timeframe, then no VLBA observations will be obtained (since a general survey of the ONC with the VLBA in a single C-band is carried out separately by Co-Is of this proposal), and the experiment will revert to its equally unique Chandra/HPF magnetic field measurements, Chandra/ALMA disk chemistry measurements, and flare-CME modeling.

psci Run:
150
 Processing Date:
Jan 3 2024
 psci Directory:
/nfs/maaxnew/r3/fl/acis126b/acis126.log
OBSID:
29117
 SIM Mode:
ACIS-I
 OTG Mode:
NONE
 Seq Number:
201581
 Target Name:
Orion_Nebula_Cl
 AO:
24
Start VCDU:
14519:000
 Start Time (UTC):
352:18558.830
 Stop Time (UTC):
352:30661.223
 Kilosecs:
12.1
 % Frames:
100.0
 # CCDs:
I4
# Frames:
3853
 # Events:
208407
 Events/sec:
17
 PSCI errors:
0
 % drops:
0.0
 Bias Errs:
0
 FP Temp:
-114.0
Parameter Block:
0x006e6034
 Window Block:
-
 # Windows:
0
 FEP Mode:
Te5x5
 BEP Mode:
F
 Start Row:
0
 # Rows:
1024
Primary Exposure:
31
 Secondary Exposure:
0
 Duty Cycle:
0
 Summing?:
No
 Bias?:
Yes
 Trickle?:
Yes
 Bias Run:
150

pgf@space.mit.edu Mon Mar 31 10:36:39 EST 2025