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The Cosmic Dance of SAX J1808.4-3658

SAX J1808.4-3658 reveals mysteries of neutron stars and their companion relationships.

L. Asquini, M. C. Baglio, S. Campana, P. D'Avanzo, A. Miraval Zanon, K. Alabarta, D. M. Russell, D. M. Bramich

― 5 min read


Mysteries of SAX Mysteries of SAX J1808.4-3658 optical behavior. Neutron star system reveals unexpected
Table of Contents

SAX J1808.4-3658 is a binary system that includes a neutron star and a companion star. They are like dance partners in space, with the neutron star being the compact and heavy one, while the companion is smaller and contributes material. This material is pulled from the companion star, forming a swirling disk around the neutron star. It's a bit of a cosmic recycling program going on!

What Makes SAX J1808 Special?

What makes SAX J1808 particularly interesting is that it can suddenly brighten up in X-rays. Think of it like a star that sometimes gets really excited and wants to show off! This system has been known to flare up, sometimes making it a target for astronomers who want to see what happens.

The fascinating part is how often SAX J1808 goes into these exciting states. Since being discovered, it has had a series of Outbursts, like a seasonal sports team that wins every few years. Each outburst brings a surge of light and X-ray energy, making it a thrilling spectacle for those observing from Earth.

The 2019 Outburst

In 2019, SAX J1808 went through another one of its outburst episodes. This time, it was slightly different, as both X-ray and optical (visible light) Observations were made. This allowed scientists to get a better picture of what was happening.

The outburst peaked on August 10, and by August 24, things became even more interesting. The system entered what scientists call a "reflaring" phase, where brightness would increase again after the initial peak, like a second act in a play.

Observations and Data Collection

Astronomers used powerful tools like the Very Large Telescope to gather data. They took lots of different measurements of the light coming from SAX J1808, hoping to see how it changed over time.

These measurements help scientists understand not just the brightness but also the different types of light (like UV and optical) coming from the system. It's like gathering all the ingredients needed to bake a cake, where each type of light represents a different flavor.

Spectroscopy: The Science of Light

One key technique used in these observations is called spectroscopy. This fancy word simply means that scientists break down light into its different colors (or wavelengths). By doing this, they can see if there are any 'fingerprints'-specific lines or marks-that tell them what chemicals or materials are present in the light.

During the 2019 outburst, the scientists expected to see certain features, like Emission Lines, which are like musical notes in the light spectrum. However, to their surprise, things looked unusually quiet. Instead of the expected vibrant symphony of colors, it was more like a muted piano solo.

Missing Emission Lines: What Happened?

The lack of emission lines in the optical spectrum during the reflaring phase was puzzling. Normally, these lines would indicate various elements present in the system-a bit like reading the ingredients list on a cereal box. But here, it was as if important ingredients were suddenly missing!

Two main ideas were proposed to explain this mystery.

1. An Emptied Disk

The first thought is that the inner part of the swirling disk around the neutron star might be empty. If the material was all used up during the initial outburst, there might not be enough left for those telltale lines to show up. It’s similar to icing on a cake; if you eat all the frosting, there’s none left for the decoration!

2. Jet Emission

The second possibility is that the neutron star was sending out Jets of particles-kind of like a cosmic firework show! These jets can affect the light we see, potentially washing out certain features. In this case, the lines we expect could be overshadowed by the extra light from the jets.

Why This Matters

Understanding why SAX J1808 behaves the way it does gives scientists clues about how neutron stars and their Disks work. It's a bit like figuring out the secret recipe behind your favorite dish-every detail matters!

By studying these systems, astronomers learn more about the end stages of stellar evolution and the incredible interactions between stars. This knowledge adds to our understanding of the universe, helping scientists piece together the cosmic puzzle.

How Do We Fit This Together?

Through the observations made during the 2019 outburst, scientists can create models to explain the behavior of SAX J1808. These models help illustrate how the components of the system interact, which is crucial for making sense of what we see in our telescopes.

Imagine trying to solve a jigsaw puzzle where some pieces are missing. Using collected data, scientists can theorize what those missing pieces might look like and how they fit into the overall picture. Each observation adds a little more clarity to the final image.

Conclusion: A Cosmic Mystery

SAX J1808.4-3658 continues to be an exciting area of study in astronomy. The strange behavior of its optical spectra during the 2019 outburst adds to the intrigue.

As scientists continue to gather data and refine their models, they chip away at the mystery. Who knows what they will find next? Maybe they'll discover that, like a good plot twist in a movie, this system has more surprises in store for us.

In the end, the universe is filled with wonders, and SAX J1808 is just one of many fascinating stories waiting to be told. So next time you look at the night sky, remember that behind those twinkling stars, exciting tales are unfolding, full of cosmic drama, unexpected turns, and perhaps even a bit of humor if the universe decides to play along!

Original Source

Title: Lack of emission lines in the optical spectra of SAX J1808.4-3658 during reflaring of the 2019 outburst

Abstract: We present spectroscopy of the accreting X-ray binary and millisecond pulsar SAX J1808.4-3658. These observations are the first to be obtained during a reflaring phase. We collected spectroscopic data during the beginning of reflaring of the 2019 outburst and we compare them to previous datasets, taken at different epochs both of the same outburst and across the years. In order to do so, we also present spectra of the source taken during quiescence in 2007, one year before the next outburst. We made use of data taken by the Very Large Telescope (VLT) X-shooter spectrograph on August 31, 2019, three weeks after the outburst peak. For flux calibration, we used photometric data taken during the same night by the 1m telescopes from the Las Cumbres Observatory network that are located in Chile. We compare our spectra to the quiescent data taken by the VLT-FORS1 spectrograph in September 2007. We inspected the spectral energy distribution by fitting our data with a multi-colour accretion disk model and sampled the posterior probability density function for the model parameters with a Markov-Chain Monte Carlo algorithm. We find the optical spectra of the 2019 outburst to be unusually featureless, with no emission lines present despite the high resolution of the instrument. Fitting the UV-optical spectral energy distribution with a disk plus irradiated star model results in a very large value for the inner disk radius of $\sim 5130 \pm 240$ km, which could suggest that the disk has been emptied of material during the outburst, possibly accounting for the emission-less spectra. Alternatively, the absence of emission lines could be due to a significant contribution of the jet emission at optical wavelengths.

Authors: L. Asquini, M. C. Baglio, S. Campana, P. D'Avanzo, A. Miraval Zanon, K. Alabarta, D. M. Russell, D. M. Bramich

Last Update: 2024-11-07 00:00:00

Language: English

Source URL: https://arxiv.org/abs/2411.04828

Source PDF: https://arxiv.org/pdf/2411.04828

Licence: https://creativecommons.org/licenses/by/4.0/

Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.

Thank you to arxiv for use of its open access interoperability.

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