Parkes observations for project P878 semester 2014OCTS
Measuring the magnetic field and electron density of the solar wind is essential in order to understand the properties of solar corona. Detection of dispersion measure (DM) and Faraday rotation measure (RM) of linearly polarized radio sources occulted by the solar wind provides a unique opportunity...
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Online Access: | https://researchdata.ands.org.au/parkes-observations-project-semester-2014octs/663496 |
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ftands:oai:ands.org.au::663496 2023-05-15T18:22:45+02:00 Parkes observations for project P878 semester 2014OCTS xiaopeng You (hasPrincipalInvestigator) CSIRO (isManagedBy) Temporal: From 2014-10-01 to 2015-03-31 https://researchdata.ands.org.au/parkes-observations-project-semester-2014octs/663496 unknown Commonwealth Scientific and Industrial Research Organisation https://researchdata.ands.org.au/parkes-observations-project-semester-2014octs/663496 102.100.100/21627 https://data.csiro.au/dap/ pulsars neutron stars interstellar medium in and around the Milky Way magnetic fields Astronomical and Space Sciences not elsewhere classified PHYSICAL SCIENCES ASTRONOMICAL AND SPACE SCIENCES dataset ftands 2020-01-05T20:51:54Z Measuring the magnetic field and electron density of the solar wind is essential in order to understand the properties of solar corona. Detection of dispersion measure (DM) and Faraday rotation measure (RM) of linearly polarized radio sources occulted by the solar wind provides a unique opportunity to measure these properties. Pulsars are therefore ideal sources for such study, especially for millisecond pulsars which can be used to obtain high timing precision to measure the DM variations caused by the solar wind. Two millisecond pulsars, PSRs J1730-2304 and J1824-2452A with ecliptic latitude of only 0.19 and -1.55 degree are ideal for this work as the line-of-sight to these pulsars goes very close to the Sun; the closest approach is only 0.8 and 5.8 solar radii respectively. We can use these two pulsars detect the different regions of the solar coronal, such as solar equator and south pole region. We also propose a unique study of the solar corona on small physical scales using the lines-of-sight to multiple pulsars in the M28 globular cluster. Dataset South pole Research Data Australia (Australian National Data Service - ANDS) Faraday ENVELOPE(-64.256,-64.256,-65.246,-65.246) Milky Way ENVELOPE(-68.705,-68.705,-71.251,-71.251) South Pole |
institution |
Open Polar |
collection |
Research Data Australia (Australian National Data Service - ANDS) |
op_collection_id |
ftands |
language |
unknown |
topic |
pulsars neutron stars interstellar medium in and around the Milky Way magnetic fields Astronomical and Space Sciences not elsewhere classified PHYSICAL SCIENCES ASTRONOMICAL AND SPACE SCIENCES |
spellingShingle |
pulsars neutron stars interstellar medium in and around the Milky Way magnetic fields Astronomical and Space Sciences not elsewhere classified PHYSICAL SCIENCES ASTRONOMICAL AND SPACE SCIENCES Parkes observations for project P878 semester 2014OCTS |
topic_facet |
pulsars neutron stars interstellar medium in and around the Milky Way magnetic fields Astronomical and Space Sciences not elsewhere classified PHYSICAL SCIENCES ASTRONOMICAL AND SPACE SCIENCES |
description |
Measuring the magnetic field and electron density of the solar wind is essential in order to understand the properties of solar corona. Detection of dispersion measure (DM) and Faraday rotation measure (RM) of linearly polarized radio sources occulted by the solar wind provides a unique opportunity to measure these properties. Pulsars are therefore ideal sources for such study, especially for millisecond pulsars which can be used to obtain high timing precision to measure the DM variations caused by the solar wind. Two millisecond pulsars, PSRs J1730-2304 and J1824-2452A with ecliptic latitude of only 0.19 and -1.55 degree are ideal for this work as the line-of-sight to these pulsars goes very close to the Sun; the closest approach is only 0.8 and 5.8 solar radii respectively. We can use these two pulsars detect the different regions of the solar coronal, such as solar equator and south pole region. We also propose a unique study of the solar corona on small physical scales using the lines-of-sight to multiple pulsars in the M28 globular cluster. |
author2 |
xiaopeng You (hasPrincipalInvestigator) CSIRO (isManagedBy) |
format |
Dataset |
title |
Parkes observations for project P878 semester 2014OCTS |
title_short |
Parkes observations for project P878 semester 2014OCTS |
title_full |
Parkes observations for project P878 semester 2014OCTS |
title_fullStr |
Parkes observations for project P878 semester 2014OCTS |
title_full_unstemmed |
Parkes observations for project P878 semester 2014OCTS |
title_sort |
parkes observations for project p878 semester 2014octs |
publisher |
Commonwealth Scientific and Industrial Research Organisation |
url |
https://researchdata.ands.org.au/parkes-observations-project-semester-2014octs/663496 |
op_coverage |
Temporal: From 2014-10-01 to 2015-03-31 |
long_lat |
ENVELOPE(-64.256,-64.256,-65.246,-65.246) ENVELOPE(-68.705,-68.705,-71.251,-71.251) |
geographic |
Faraday Milky Way South Pole |
geographic_facet |
Faraday Milky Way South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
https://data.csiro.au/dap/ |
op_relation |
https://researchdata.ands.org.au/parkes-observations-project-semester-2014octs/663496 102.100.100/21627 |
_version_ |
1766202167224434688 |