Gustavo E. Romero

Last updated
Gustavo Esteban Romero
Dr. Gustavo Romero.jpg
Born (1964-09-20) 20 September 1964 (age 59)
La Plata, Buenos Aires
Scientific career
FieldsRelativistic Astrophysics.
Institutions University of La Plata

Gustavo E. Romero is a professor of Relativistic Astrophysics at the University of La Plata in Argentina. In addition to his academic role, he serves as a Superior Researcher of the National Research Council of Argentina. [1] Romero also holds the position of Director of the Argentine Institute of Radio Astronomy (IAR). Additionally, Romero has previously served as President of the Argentine Astronomical Society [2] and is currently the leader of the GARRA research group [3] and a Helmholtz International Fellow. [4]

Contents

For his professional accomplishments, Romero has been honored with several notable awards in scientific research, including an award from the Argentine Academy of Sciences, [5] the Houssay Prize [6] and the Konex Award 2023. [7]

Research work

Romero has worked extensively on gamma-ray, neutrino and cosmic-ray astrophysics, black holes, and scientific philosophy. He is well known for his investigations of blazars, microquasars, and unidentified gamma-ray sources. [8] His research has received around 11000 citations in the academic literature, [9] making him one of the most cited scientists of Argentina. [10]


In the field of philosophy, he has contributed with research on Supertask, spacetime ontology, [11] and aesthetics. [12] Romero is usually considered a disciple of the Argentine-Canadian philosopher and physicist Mario Bunge . [13]


Selected publications


Books

Related Research Articles

<span class="mw-page-title-main">Gamma-ray burst</span> Flashes of gamma rays from distant galaxies

In gamma-ray astronomy, gamma-ray bursts (GRBs) are immensely energetic explosions that have been observed in distant galaxies, described by NASA as "the most powerful class of explosions in the universe". They are the most energetic and luminous electromagnetic events since the Big Bang. Bursts can last from ten milliseconds to several hours. After an initial flash of gamma rays, a longer-lived "afterglow" is usually emitted at longer wavelengths.

<span class="mw-page-title-main">X-ray binary</span> Class of binary stars

X-ray binaries are a class of binary stars that are luminous in X-rays. The X-rays are produced by matter falling from one component, called the donor, to the other component, called the accretor, which is either a neutron star or black hole. The infalling matter releases gravitational potential energy, up to 30 percent of its rest mass, as X-rays. The lifetime and the mass-transfer rate in an X-ray binary depends on the evolutionary status of the donor star, the mass ratio between the stellar components, and their orbital separation.

Soft X-ray transients (SXTs), also known as X-ray novae and black hole X-ray transients, are composed of a compact object and some type of "normal", low-mass star. These objects show dramatic changes in their X-ray emission, probably produced by variable transfer of mass from the normal star to the compact object, a process called accretion. In effect the compact object "gobbles up" the normal star, and the X-ray emission can provide the best view of how this process occurs. The "soft" name arises because in many cases there is strong soft X-ray emission from an accretion disk close to the compact object, although there are exceptions which are quite hard.

<span class="mw-page-title-main">Astrophysical jet</span> Beam of ionized matter flowing along the axis of a rotating astronomical object

An astrophysical jet is an astronomical phenomenon where outflows of ionised matter are emitted as extended beams along the axis of rotation. When this greatly accelerated matter in the beam approaches the speed of light, astrophysical jets become relativistic jets as they show effects from special relativity.

<span class="mw-page-title-main">SS 433</span> Binary star system in the constellation Aquila

SS 433 is a microquasar or eclipsing X-ray binary system, consisting of a stellar-mass black hole accreting matter from an A-type companion star. SS 433 is the first discovered microquasar. It is at the centre of the supernova remnant W50.

Cygnus X-3 is a high-mass X-ray binary (HMXB), one of the stronger binary X-ray sources in the sky. It is often considered to be a microquasar, and it is believed to be a compact object in a binary system which is pulling in a stream of gas from an ordinary star companion. It is one of only two known HMXBs containing a Wolf–Rayet star. It is invisible visually, but can be observed at radio, infrared, X-ray, and gamma-ray wavelengths.

The Tolman–Oppenheimer–Volkoff limit is an upper bound to the mass of cold, non-rotating neutron stars, analogous to the Chandrasekhar limit for white dwarf stars. Stars more massive than the TOV limit collapse into a black hole. The original calculation in 1939, which neglected complications such as nuclear forces between neutrons, placed this limit at approximately 0.7 solar masses (M☉). Later, more refined analyses have resulted in larger values.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

LS I +61 303 is a microquasar, a binary system containing a massive star and a compact object. The compact object is a pulsar and the system is around 7,000 light-years away.

<span class="mw-page-title-main">LS 5039</span> Binary star system in the constellation Scutum

LS 5039 is a binary system in the constellation of Scutum. It has an apparent magnitude of 11.27, and it is about 8,200 light-years away.

GCIRS 13E is an infrared and radio object near the Galactic Center. It is believed to be a cluster of hot massive stars, possibly containing an intermediate-mass black hole (IMBH) at its center.

The Whole Earth Blazar Telescope (WEBT) is an international consortium of astronomers created in 1997, with the aim to study a particular category of Active Galactic Nuclei (AGN) called blazars, which are characterized by strong and fast brightness variability, on time scales down to hours or less.

GRB 011211 was a gamma-ray burst (GRB) detected on December 11, 2001. A gamma-ray burst is a highly luminous flash associated with an explosion in a distant galaxy and producing gamma rays, the most energetic form of electromagnetic radiation, and often followed by a longer-lived "afterglow" emitted at longer wavelengths.

<span class="mw-page-title-main">HD 5980</span> Triple star system in the constellation Tucana

HD 5980 is a multiple star system on the outskirts of NGC 346 in the Small Magellanic Cloud (SMC) and is one of the brightest stars in the SMC.

<span class="mw-page-title-main">X Persei</span> Variable star in the constellation Perseus

X Persei is a high-mass X-ray binary system located in the constellation Perseus, approximately 950 parsecs away. It is catalogued as 4U 0352+309 in the final Uhuru catalog of X-ray objects.

<span class="mw-page-title-main">Markarian 501</span> Elliptical galaxy emitting very-high-energy gamma rays

Markarian 501 is a galaxy with a spectrum extending to the highest energy gamma rays. It is a blazar or BL Lac object, which is an active galactic nucleus with a jet that is shooting towards the Earth. The object has a redshift of z = 0.034.

HD 93403 is a spectroscopic binary containing two highly luminous hot blue stars. It is 10,000 light years away in the Carina Nebula in the constellation Carina. It appears to have spectral type O5.5III, but this is composed of two spectra from a blue supergiant and blue main sequence star of spectral type O5.5I and O7V respectively. The two stars orbit every 15 days with a separation that varies from 93 R☉ to 149 R☉. The binary is shedding mass at the high rate of 0.0005 M☉ per year.

<span class="mw-page-title-main">V4024 Sagittarii</span> Star in the constellation Sagittarius

V4024 Sagittarii is a single variable star in the southern constellation of Sagittarius. It has a blue-white hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates from about 5.3 to 5.6. The star is located at a distance of approximately 1,700 light years based on stellar parallax, but is drifting closer with a radial velocity of −20 km/s. The position of this star near the ecliptic means it is subject to lunar occultations.

<span class="mw-page-title-main">XTE J1118+480</span> Star system in the constellation Ursa Major

XTE J1118+480 is a low-mass X-ray binary in the constellation Ursa Major. It is a soft X-ray transient that most likely contains a black hole and is probably a microquasar.

<span class="mw-page-title-main">AP Librae</span> Active galactic nucleus in the constellation Libra

AP Librae is a BL Lacertae object located at a distance of 700 million light years in the southern constellation of Libra. In the visual band it is one of the most active blazars known. AP Lib is surrounded by an extended source with a spectrum characteristic of a red-shifted giant elliptical galaxy. The derived visual magnitude of this region is 15.0, and it follows a radially decreasing brightness that is characteristic of an elliptical. Seven fainter galaxies are visible within an angular radius of 9′, suggesting it is the brightest member of a galactic cluster.

References

  1. ↑ "National Research Council of Argentina". conicet.gov (in Spanish).
  2. ↑ "Argentine Astronomical Society". astronomiaargentina.org.ar (in Spanish).
  3. ↑ "GARRA". GRUPO DE ASTROFÍSICA RELATIVISTA Y RADIOASTRONOMÍA.
  4. ↑ "Helmholtz International Fellow Award für weitere fünf Wissenschaftler". Helmholtz.de (in German).[ dead link ]
  5. ↑ "Award of the Argentine Academy of Sciences" (in Spanish). 8 June 2020.
  6. ↑ "Houssay Prize" (in Spanish). 9 April 2019.
  7. ↑ Fundación Konex (2 May 2023). "Premios Konex 2023: Ciencia y Tecnología. Ya se conocen los Diplomas al Mérito". fundacionkonex.org (in Spanish). Retrieved 2023-05-15.
  8. ↑ Romero, Gustavo E. (December 2005). "Microquasars and Gamma-ray Sources". Chinese Journal of Astronomy and Astrophysics. 5: 110–120. doi:10.1088/1009-9271/5/S1/110. hdl: 11336/29696 . S2CID   15373413.
  9. ↑ "Google Scholar".
  10. ↑ "Webometrics". www.webometrics.info.
  11. ↑ Romero, Gustavo E. (2017). "On the Ontology of Spacetime: Substantivalism, Relationism, Eternalism, and Emergence". Foundations of Science. 22: 141–159. doi:10.1007/s10699-015-9476-1. hdl: 11336/35354 . S2CID   124842203.
  12. ↑ Romero, Gustavo E. (2018). "Outline of a Theory of Scientific Aesthetics". Foundations of Science. 23 (4): 795–807. doi:10.1007/s10699-018-9551-5. S2CID   126062553.
  13. ↑ Bunge, Mario (2016). Between Two Worlds Memoirs of a Philosopher-Scientist. doi:10.1007/978-3-319-29251-9. ISBN   978-3-319-29250-2.
  14. ↑ Romero, G. E.; Torres, D. F.; Kaufman Bernadó, M. M.; Mirabel, I. F. (2003). "Hadronic gamma-ray emission from windy microquasars". Astronomy & Astrophysics. 410 (2): L1–L4. arXiv: astro-ph/0309123 . Bibcode:2003A&A...410L...1R. doi: 10.1051/0004-6361:20031314-1 .
  15. ↑ "Unidentified 3eg gamma-ray sources at low galactic latitude". arXiv: astro-ph/9904355 .
  16. ↑ Romero, G. E.; Cellone, S. A.; Combi, J. A. (1999). "Optical microvariability of southern AGNs". Astronomy and Astrophysics Supplement Series. 135 (3): 477–486. Bibcode:1999A&AS..135..477R. doi: 10.1051/aas:1999184 .
  17. ↑ Romero, G. E.; Okazaki, A. T.; Orellana, M.; Owocki, S. P. (2007). "Accretion vs. colliding wind models for the gamma-ray binary LS I+ 61 303: an assessment". Astronomy & Astrophysics. 474 (1): 15–22. arXiv: 0706.1320 . Bibcode:2007A&A...474...15R. doi: 10.1051/0004-6361:20078035 .
  18. ↑ Benaglia, P.; Romero, G. E. (2003). "Gamma-ray emission from Wolf-Rayet binaries". Astronomy & Astrophysics. 399 (3): 1121–1134. arXiv: astro-ph/0205375 . Bibcode:2003A&A...399.1121B. doi: 10.1051/0004-6361:20021854 .
  19. ↑ Eiroa, Ernesto F.; Romero, Gustavo E.; Torres, Diego F. (2002). "Reissner-Nordström black hole lensing". Physical Review D. 66 (2): 024010. arXiv: gr-qc/0203049 . Bibcode:2002PhRvD..66b4010E. doi:10.1103/PhysRevD.66.024010. S2CID   12504121.
  20. ↑ Torres, D. (2003). "Supernova remnants and γ-ray sources". Physics Reports. 382 (6): 303–380. arXiv: astro-ph/0209565 . Bibcode:2003PhR...382..303T. doi:10.1016/S0370-1573(03)00201-1. hdl: 11336/30888 . S2CID   54074190.
  21. ↑ Eiroa, Ernesto F.; Romero, Gustavo E. (2004). "Linearized stability of charged thin-shell wormholes". General Relativity and Gravitation. 36 (4): 651–659. arXiv: gr-qc/0303093 . Bibcode:2004GReGr..36..651E. doi:10.1023/B:GERG.0000016916.79221.24. hdl: 11336/29923 . S2CID   119367195.
  22. ↑ Romero, Gustavo E.; Christiansen, Hugo R.; Orellana, Mariana (2005). "Hadronic high-energy gamma-ray emission from the microquasar LS I+ 61 303". The Astrophysical Journal. 632 (2): 1093–1098. arXiv: astro-ph/0506735 . Bibcode:2005ApJ...632.1093R. doi:10.1086/444446. hdl: 11336/29928 . S2CID   15582485.
  23. ↑ Introduction to Black Hole Astrophysics. Lecture Notes in Physics. Vol. 876. 2014. doi:10.1007/978-3-642-39596-3. ISBN   978-3-642-39595-6.
  24. ↑ Romero, Gustavo E. (2018). Scientific Philosophy. Bibcode:2018scph.book.....R. doi:10.1007/978-3-319-97631-0. ISBN   978-3-319-97630-3.
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