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Дата изменения: Tue Sep 15 04:38:05 2015
Дата индексирования: Mon Apr 11 16:44:16 2016
Кодировка:
Поисковые слова: annular solar eclipse

Proposal Identification No.:

A3020 Arecibo Observatory

Date Received: 2015-Sep-01 12:53:12 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2015. This proposal has not been submitted before. Proposal Type: General Category: Observation Category: Time Requested this semester: Hours already used for this pro ject: Additional Hours required to complete pro ject: Minimum Useful Time: Expected Data Storage: Prop osal Title: Regular Astronomy 61.5

2.5 hours 100-500 GB

AN UPDATED PROPOSAL TO MEASURE MAGNETIZED ELECTRON DENSITY FLUCTUATIONS IN MIRA-VARIABLE-STAR CORONAE
ABSTRACT: We have recently realized a technique for measuring electron density fluctuations in the Sun's corona and found many interesting results, including: periodic fluctuations in electron column density; Coronal Mass Ejection (CME) magnetized electron clouds; turbulent spectra; power transfer from circular to linear polarization. The technique uses the propagation effects on a spacecraft downlink carrier. The goal of this proposal is to explore propagation effects in the coronae of Mira variable stars, using the OH maser lines on the far side of the star (i.e., the positive-velocity masers) as the signal. This is completely unexplored territory in stars. If we are successful, we may open up a new observational field--the exploration and characterization of physical conditions and activity in stellar coronae. Outreach Abstract: We have recently realized a technique for measuring electron density fluctuations in the Sun's corona and found many interesting results, including: periodic fluctuations in electron column density; Coronal Mass Ejection (CME) magnetized electron clouds; turbulent spectra; power transfer from circular to linear polarization. The technique uses the propagation effects on a spacecraft downlink carrier. The goal of this proposal is to explore propagation effects in the coronae of Mira variable stars, using the OH maser lines on the far side of the star (i.e., the positive-velocity masers) as the signal. This is completely unexplored territory in stars. If we are successful, we may open up a new observational field--the exploration and characterization of physical conditions and activity in stellar coronae.

Name carl Heiles Murray Lewis

Institution Univ of Calif Berkeley arecibo observatory

E-mail heiles@astro.berkeley.edu bmllewis@gmail.com

Phone 510 280 8099 787 890 5010

Student no no

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Additional Authors
Adam Kobelski,National Radio Astronomy Observatory akobelsk@nrao.edu Elizabeth JensenPlanetary Science Institute Ejensen@psi.edu David Wexler, University of Southern Queensland (graduate student in Astronomy) dwexler@mit.edu (visiting student MIT Haystack Observatory)

This work is part of a MS thesis.

Remote Observing Request

Observer will travel to AO X Remote Observing In Absentia (instructions to operator)

Section I I - Time Request
The following times are in LST. For these observations night-time is not needed.

Begin End IntervalInterval

Days Needed at This Interval 3

Time Constraints (Must Be Justified in the Prop osal Text) 3 full transits on each source except for W49, with the three observing days spaced close together. For W49, three sessions of 30 minutes each. Name Ra Dec RiseTime SetTime 01037+1219 01:06:25.9 12:35:54.1 23:48:56 02:25:37 03507+1115 03:53:28.6 11:24:19.7 02:37:56 05:10:45 06500+0829 06:52:46.9 8:25:20.0 05:43:39 08:03:36 07331+0021 07:35:41.2 0:14:58.7 07:05:18 08:07:39 15255+1944 15:27:47.2 19:33:48.4 14:05:19 16:51:39 17579+2335 18:00:03.7 23:35:35.7 16:39:19 19:22:07 2

18069+0911 18:09:18.4 9:12:15.5 16:58:08 19:22:00 20406+2953 20:42:45.9 30:04:06.0 19:33:58 21:52:55 W49 19:07:53 09:01:00 17:57:06 20:12:12 Regarding day/night: The only reason to require night time is because of IRIDIUM. The observations are extremely narrow band and might not be affected. We are willing to try a test observation during the day to see if IRIDIUM is a problem.

Section I I I - Instruments Needed
L-wide Atmospheric Observation Instruments:

Sp ecial Equipment or setup: Mock spectrometers

Section IV - RFI Considerations Frequency Ranges Planned
1612 1665 1667 1720 This proposal requires Iridium RFI protection at 1612 MHz between 10pm and 6am EST.

Section V - Observing List Target List
See Table 2 in 'time request' section.

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