Institutional Repository of Radio Astronomy Research Laboratory
| Visibility of Pulsar Emission: Motion of the Visible Point | |
Yuen, R.1,2,3 ; Melrose, D. B.1
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| 2014-10-08 | |
| Source Publication | PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
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| Volume | 31Pages:e039 |
| Contribution Rank | 3 |
| Abstract | A standard model for the visibility of pulsar radio emission is based on the assumption that the emission is confined to a narrow cone about the tangent to a dipolar field line. The widely accepted rotating vector model (RVM) is an approximation in which the line of sight is fixed and the field line is not strictly tangent to it. We refer to an exact treatment (Gangadhara, 2004) as the tangent model. In the tangent model (but not in the RVM) the visible point changes as a function of pulsar rotational phase, psi, defining a trajectory on a sphere of radius r. We solve for the trajectory and for the angular velocity of the visible point around it. We note the recent claim that this motion is observable using interstellar holography (Pen et al., 2014). We estimate the error introduced by use of the RVM and find that it is significant for pulsars with emission over a wide range of psi. The RVM tends to underestimate the range of psi over which emission is visible. We suggest that the geometry alone strongly favors the visible pulsar radio being emitted at a heights more than ten percent of the light-cylinder distance, where our neglect of retardation effects becomes significant. |
| Keyword | Radiation Mechanisms: Non-thermal Pulsar: General |
| Subtype | Article |
| DOI | 10.1017/pasa.2014.35 |
| WOS Headings | Science & Technology ; Physical Sciences |
| Indexed By | SCI |
| Language | 英语 |
| WOS Keyword | RADIO-EMISSION ; POLARIZATION ; RADIATION ; ALTITUDE ; MODEL |
| WOS Research Area | Astronomy & Astrophysics |
| WOS Subject | Astronomy & Astrophysics |
| WOS ID | WOS:000342737900001 |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/606 |
| Collection | 射电天文研究室_脉冲星研究团组 射电天文研究室 |
| Affiliation | 1.Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia 2.Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia 3.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China |
| First Author Affilication | Xinjiang Astronomical Observatory, Chinese Academy of Sciences |
| Recommended Citation GB/T 7714 | Yuen, R.,Melrose, D. B.. Visibility of Pulsar Emission: Motion of the Visible Point[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA,2014,31:e039. |
| APA | Yuen, R.,&Melrose, D. B..(2014).Visibility of Pulsar Emission: Motion of the Visible Point.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA,31,e039. |
| MLA | Yuen, R.,et al."Visibility of Pulsar Emission: Motion of the Visible Point".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA 31(2014):e039. |
| Files in This Item: | ||||||
| File Name/Size | DocType | Version | Access | License | ||
| Visibility of Pulsar（1097KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-ND | View Application Full Text | |
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