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Дата изменения: Tue Sep 9 17:24:53 2014
Дата индексирования: Mon Apr 11 16:43:48 2016
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Поисковые слова: п п п п п п п п п п п п п п п п п п п п п
Proposal Identification No.:

P2822 Arecibo Observatory

Date Received: 2014-Sep-02 11:26:16 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2014. This proposal has been submitted before. The previous proposal number is P2822. Proposal Type: General Category: Observation Category: Time Requested this semester: Hours Next Semester: Hours already used for this pro ject: Additional Hours required to complete pro ject: Minimum Useful Time: Expected Data Storage: Prop osal Title: ABSTRACT: Regular Pulsars Galactic 7 6 80+ 36? 1 hour less than 100 GB

Continued Timing of a Millisecond Pulsar in a Stellar Triple System

The millisecond pulsar hierarchical triple system PSR J0337+1715 has gotten much more exciting over the past year, thanks in large part to the high-precision of Arecibo timing observations. We now have a full high-precision timing solution of the system, with the timing model based on accurate three-body gravitational simulations. The model has provided the orbital inclinations and masses of all three stars to high precision. Over the coming year we will measure secular changes to the orbits due to three-body effects and will make by far the best test of the Strong Equivalence Principle (SEP) to date. This test will have important implications for basic physics, and the >50% extension to the high-precision Arecibo/PUPPI timing baseline will be critical for setting a tight and robust limit on SEP violations. Outreach Abstract: The millisecond pulsar triple system PSR J0337+1715 has gotten much more exciting over the past year, thanks in large part to the high-precision of Arecibo timing observations. We now have a precise model of the system based on three-body gravitational calculations. The model gives us the orbital inclinations and masses of all three stars, a neutron star and two white dwarfs, to high precision. Over the coming year we will measure slow changes to the orbits due to complicated three-body gravitational effects and will make by far the best test of the Strong Equivalence Principle (SEP) to date. This test will have important implications for basic physics, including a new test of Einstein's general relativity.

Name Scott M Ransom Duncan Lorimer

Institution NRAO West Virginia University

E-mail sransom@nrao.edu Duncan.Lorimer@mail.wvu.edu

Phone (434) 296-0320 (304) 293-3422

Student no no

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Additional Authors
Anne Archibald Jason Hessels David Kaplan Ryan Lynch Ingrid Stairs

This work is not part of a 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 03:00 ­ 04:00 ­ ­ ­

Days Needed at This Interval 7

Time Constraints (Must Be Justified in the Prop osal Text) Observations should be spaced roughly four weeks apart and run for one year.

Next Semester Time Request

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Begin ­ End Interval­Interval 03:00 ­ 04:00 ­ ­ ­

Days Needed at This Interval 6

Time Constraints (Must Be Justified in the Prop osal Text) Same as above: approx 4 weeks between observations.

Section I I I - Instruments Needed
430 G L-wide

Atmospheric Observation Instruments:

Sp ecial Equipment or setup: We will only use PUPPI.

Section IV - RFI Considerations Frequency Ranges Planned
All of L-wide with PUPPI. This proposal requires coordination with Punta Salinas radar within the band 1222-1381 MHz.. This proposal requires coordination with GPS L3 at 1381 MHz.

Section V - Observing List Target List
PSR J0337+1717 visible 02:15-05:00 LST

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