Chandra Large, Very Large and X-ray Visionary Projects

WD BINARES & CV

Proposal Number	Subject Category	PI Name	Type	Time (ks)	Title
08300134	WD BINARIES AND CV	Hoogerwerf	LP	500	Testing the Physics of Magnetic Accretion: EX Hydrae from the Shock to the White Dwarf Surface
09300101	WD BINARIES AND CV	Pooley	LP	437.5	A Chandra Legacy Survey of Dynamically Active Globular Clusters
12300901	WD BINARIES AND CV	SOKOLOSKI	LP	650	X-RAY IMAGING OF NOVA SHELLS

Subject Category: WD BINARIES AND CV

Proposal Number: 08300134

Title: Testing the Physics of Magnetic Accretion: EX Hydrae from the Shock to the White Dwarf Surface

Type: LP Total Time: 500

PI Name: Ronnie Hoogerwerf

We propose to observe the magnetic Cataclysmic Variable (CV) EX Hydrae with the HETG to make a direct measurement of the temperature and density structure of its accretion columns and study the physics of the shock and subsequent cooling flow. The accretion column structure, crucial to our understanding of accretion physics, remains one of the last unexplored components of CVs and other accreting objects. The accretion columns of EX Hydrae are unobscured and are periodically occulted by the body of the white dwarf, making it the ideal target for this study. We will use high signal-to-noise light curves for individual spectral lines to measure the temperature and density structure. The result will be applicable to a broad range of objects from clusters of galaxies to T Tauri stars.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
12:52:24.20	-29:14:56.70	EX Hydrae	ACIS-S	HETG	500

Subject Category: WD BINARIES AND CV

Proposal Number: 09300101

Title: A Chandra Legacy Survey of Dynamically Active Globular Clusters

Type: LP Total Time: 437.5

PI Name: David Pooley

From our experience with Chandra, we have determined an empirical, successful, and model-independent method for determining the the neutron-star low-mass X-ray binary (LMXB) content and bright cataclysmic variable (CV) of a globular cluster (GC) in a reasonably short ACIS exposure. We propose a program that will discover ~30 LMXBs and ~150 CVs in 31 GCs. When combined with other observations, we will have direct knowledge of over 90% of the total LMXB population in GCs. We will accurately determine the role of GC dynamics in the formation of both LMXBs and CVs. We will also obtain an estimate for the density of the LMXBs and CVs in the field. This study will have important implications both for theories of LMXB and CV formation and for theories of GC dynamics and evolution.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
19:18:02.10	+18:34:18.00	Pal 10	ACIS-S	NONE	11.2
18:31:23.20	-32:20:53.00	NGC 6637	ACIS-S	NONE	7.3
17:37:36.10	-03:14:45.00	NGC 6402	ACIS-S	NONE	12.2
17:38:36.60	-23:54:34.00	NGC 6401	ACIS-S	NONE	11.2
18:04:49.80	-07:35:09.00	NGC 6539	ACIS-S	NONE	14.6
18:30:56.10	-25:29:51.00	NGC 6638	ACIS-S	NONE	9
16:59:32.60	-37:07:17.00	NGC 6256	ACIS-S	NONE	9.4
17:14:32.10	-29:27:44.00	NGC 6304	ACIS-S	NONE	5.3
15:28:00.50	-50:40:22.00	NGC 5927	ACIS-S	NONE	7.7
17:19:11.80	-18:30:59.00	NGC 6333	ACIS-S	NONE	8.4
18:31:54.10	-23:28:31.00	NGC 6642	ACIS-S	NONE	7.6
18:06:08.60	-27:45:55.00	NGC 6540	ACIS-S	NONE	5
18:09:17.60	-25:54:31.00	NGC 6553	ACIS-S	NONE	5.5
18:43:12.70	-32:17:31.00	NGC 6681	ACIS-S	NONE	7.2
17:17:59.20	-23:45:57.00	NGC 6325	ACIS-S	NONE	17.9
21:33:29.30	-00:49:23.00	NGC 7089	ACIS-S	NONE	11.5
18:04:49.60	-30:03:21.00	NGC 6528	ACIS-S	NONE	12.3
17:10:10.20	-26:34:55.00	NGC 6293	ACIS-S	NONE	10
18:03:34.10	-30:02:02.00	NGC 6522	ACIS-S	NONE	8.4
13:46:26.50	-51:22:24.00	NGC 5286	ACIS-S	NONE	13.1
16:27:40.40	-38:50:56.00	NGC 6139	ACIS-S	NONE	17.8
18:01:50.60	-08:57:32.00	NGC 6517	ACIS-S	NONE	26.1
05:14:06.30	-40:02:50.00	NGC 1851	ACIS-S	NONE	19.6
17:50:12.90	-37:03:05.00	NGC 6441	ACIS-S	NONE	35.9
18:13:38.80	-31:49:37.00	NGC 6569	ACIS-S	NONE	11.2

Subject Category: WD BINARIES AND CV

Proposal Number: 12300901

Title: X-RAY IMAGING OF NOVA SHELLS

Type: LP Total Time: 650

PI Name: JENNIFER SOKOLOSKI

Novae are the most common stellar explosions in the Universe, and the most energetic after GRBs and supernovae. Like other stellar explosions, optical data show that novae are aspherical and inhomogeneous. Although novae are known to be triggered by a thermonuclear runaway (TNR) on an accreting white dwarf, the means by which the observed structure is produced is less clear. Since the shaping of nova remnants must produce shocks, and thus X-rays, Chandra imaging provides a powerful tool for understanding how novae produce their rings, clumps, and jets. We propose a major comparative study of the X-rays from nova shells to determine the processes that shape the ejecta. This work has wider implications for the physics of jets and asymmetry production in all types of stellar explosions.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time
17:50:13.20	-06:42:28.40	RS Oph	ACIS-S	NONE	250

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