Jakob Karl Ernst Halm Contents Education Career Scientific contributions References Navigation menu2014MNSSA..73...14G1907AN....173..273H10.1002/asna.190617318022004SHAN....5...13W1911MNRAS..71..610H10.1093/mnras/71.8.6101938ApJ....88..472K10.1086/1439991915MNRAS..75..150H10.1093/mnras/75.3.1501917MNRAS..77..243H10.1093/mnras/77.3.2431935JASSA...4....1H
1866 births1944 deathsSouth African astronomersUniversity of Strasbourg faculty
stellar dynamicsmass-luminosity relationUniversity Observatory, StrasbourgRoyal Observatory EdinburghRoyal Observatory, Cape of Good HopeheliometerspectrographP CygniNova PerseiCape Photographic DurchmusterungDavid GillJacobus KapteynMaxwellian distributionphotographic platesreciprocityextinctionplate tectonic theory
Jakob Karl Ernst Halm
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Jakob Karl Ernst Halm (born Bingen am Rhein: 30 November 1866 – South Africa 17 July 1944)[1][2] was a pioneer of stellar dynamics and the first person to suggest the existence of a mass-luminosity relation for stars.
Contents
1 Education
2 Career
3 Scientific contributions
4 References
Education
Halm went to school in Bingen and studied later at Giessen, Berlin and Kiel. He obtained his PhD at Kiel in 1890 for work on linear differential equations.
Career
Halm making solar observations in Edinburgh ca 1905. SAAO Archives P6694
Assistant at the University Observatory, Strasbourg (1889-1895).
First Class Assistant at the Royal Observatory Edinburgh (1895-1907).
Chief Assistant at the Royal Observatory, Cape of Good Hope (1907-1927).
Scientific contributions
While at Edinburgh Halm used a heliometer to feed a spectrograph in order to study the differential rotation of the Sun at different latitudes. He discovered that absorption lines near the edge of the Solar disc are displaced towards the red, compared with their positions at the centre. This was not due to obvious effects such as rotation.[3] He also gave the first interpretation of what is now called a P Cygni profile [4][5] while discussing the spectrum of Nova Persei 1901.
Visit of British Association group to Cape, in 1914. Halm is at back centre; Eddington at front, right. SAAO Archives (not yet catalogued)
While at the Royal Observatory, Cape of Good Hope, he was involved in follow-up work on the Cape Photographic Durchmusterung (CPD) of David Gill and Jacobus Kapteyn using radial velocities and proper motions. Repeated observations had already led to the discovery of two star streams by Kapteyn and Halm was able to identify a third (Halm 1911) associated with what he called "Orion-type" stars.[6] This paper went on to say that stars appeared to obey a Maxwellian distribution, implying equipartition of energy, i.e., the less massive ones moved more rapidly than the massive ones. His conclusion was based on stellar masses derived from a number of well-studied binaries. Eddington[7] showed, however, that stellar interactions, owing to their rarity, could not produce this result. However Halm's work was important in stimulating research on the subject.
The paper concluded that there is a relation between spectral type and mass for stars. This was the first announcement of the mass-luminosity relation, later elaborated by many others.[8]
His work on determination of magnitudes from photographic plates led him to an improved understanding of reciprocity failure, on which he published a paper,[9] leading to the Kron–Halm catenary equation.
In 1917 Halm was the first person to make an estimate of the total to selective extinction of starlight. He determined that the interstellar extinction in magnitudes is a factor of 1.22 times greater in
the blue than in the visible.[10]
Halm believed that many terrestrial features could be explained by an ongoing expansion of the earth's crust.[11] Though it created considerable interest at the time, since the advent of plate tectonic theory his expansion hypothesis is no longer considered plausible.
References
^ Glass, I.S. (2014). "Jacob Karl Ernst Halm (1865-1944)". Monthly Notes of the Astronomical Society of South Africa. 73: 14–23. Bibcode:2014MNSSA..73...14G..mw-parser-output cite.citationfont-style:inherit.mw-parser-output .citation qquotes:"""""""'""'".mw-parser-output .citation .cs1-lock-free abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .citation .cs1-lock-subscription abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registrationcolor:#555.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration spanborder-bottom:1px dotted;cursor:help.mw-parser-output .cs1-ws-icon abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/Wikisource-logo.svg/12px-Wikisource-logo.svg.png")no-repeat;background-position:right .1em center.mw-parser-output code.cs1-codecolor:inherit;background:inherit;border:inherit;padding:inherit.mw-parser-output .cs1-hidden-errordisplay:none;font-size:100%.mw-parser-output .cs1-visible-errorfont-size:100%.mw-parser-output .cs1-maintdisplay:none;color:#33aa33;margin-left:0.3em.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-formatfont-size:95%.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-leftpadding-left:0.2em.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-rightpadding-right:0.2em
^ Poggendorff, J.C. (1863) [1863 and later]. Biographisch-Literarisches Handwörterbuch. Barth.
^ Halm, J. (1907). "Über eine bisher unbekannte Verschiebung der Fraunhoferschen Linien des Sonnenspektrums". Astronomische Nachrichten. 173: 273. Bibcode:1907AN....173..273H. doi:10.1002/asna.19061731802.
^ Halm, J. (1904). "On Professor Seeliger's Theory of Temporary Stars". Proc. Roy. Soc. Edinburgh. 25: 513–552.
^ Williams, Peredur (2004). "Centenary (1904-2004) of the interpretation of the P Cygni profile". Newsletter, Society for the History of Astronomy (5): 13. Bibcode:2004SHAN....5...13W.
^ Halm, J. (1911). "Stars, motion in space, etc. Further considerations relating to the systematic motions of the stars". Monthly Notices of the Royal Astronomical Society. 71: 610–639. Bibcode:1911MNRAS..71..610H. doi:10.1093/mnras/71.8.610.
^ Eddington, A. (1914). Stellar Movements and the Structure of the Universe. Cambridge University Press.
^ Kuiper, G.P. (1938). "The Empirical Mass-Luminosity Relationship". Astrophysical Journal. 88: 472–506. Bibcode:1938ApJ....88..472K. doi:10.1086/143999.
^ Halm, J. (1915). "On the Determination of Fundamental Photographic Magnitudes". Monthly Notices of the Royal Astronomical Society. 75: 150–177. Bibcode:1915MNRAS..75..150H. doi:10.1093/mnras/75.3.150.
^ Halm, J. (1917). "On the Question of Extinction of Light in Space and the Relations between Stellar Magnitudes, Distances and Proper Motions". Monthly Notices of the Royal Astronomical Society. 77: 243–280. Bibcode:1917MNRAS..77..243H. doi:10.1093/mnras/77.3.243.
^ Halm, J. (1935). "An Astronomical Aspect of the Evolution of the Earth". Journal of the Astronomical Society of South Africa. 4: 1. Bibcode:1935JASSA...4....1H.
Categories:
- 1866 births
- 1944 deaths
- South African astronomers
- University of Strasbourg faculty
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